explanation blue bibcodes open ADS page with paths to full text
Author name code: meyer-jeanpaul
ADS astronomy entries on 2022-09-14
author:"Meyer, Jean Paul" -abs:("ATLAS" OR "boson")
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Title: Sentinel-5 OGSE: large aperture sun simulator
Authors: Mendes-Lopes, J.; Meyer, J.; Borges, P.; Pereira, J.;
Henriques, R.; Pimentao, J.; Mesquita, D.
2021SPIE11852E..4EM Altcode:
This paper reports on the development of a sun simulator (SUSI) as
an optical ground support equipment (OGSE) for the calibration and
characterization (CC) of the Sentinel-5 spectrometers. The illumination
system is based on a Xenon continuous light source, a homogenizer and
a telescope. A Xenon plasma source is significantly non-uniform, both
spectrally and spatially. To meet the stringent spatial homogeneity
requirements, a large homogenizer based on a kaleidoscope configuration
was designed and manufactured. The proper collimation and large exit
pupil are achieved through a mirror-based Offner telescope, avoiding
large incidence angles, which would affect spatial uniformity and
polarization. SUSI covers a very wide spectral range, from 270 to
2300nm, with an irradiance of 80 mW/cm2. SUSI provides an illuminated
exit pupil with a very high spatial uniformity. The collimated beam
of 0.27º divergence illuminates an exit pupil 160mm diameter with
continuous light, reaching a non-uniformity of irradiance better than 1%
for most spectrum (according to IEC 60904-9 definition) which is, to the
best of the authors' knowledge, the highest level of spatial uniformity
for large aperture sun simulators. A breadboard was manufactured to
test and validate the performance of the homogenizer coupled with the
Xenon light. Due to the large diameter of the exit pupil, a set of
tests were specifically developed to evaluate the performance across
the entire aperture and spectral range. Using a fiber-tip based
spectrometer, the exit pupil was scanned to measure the irradiance
profile. Results from the breadboard showed a performance better
than 1% spatial uniformity at 0.27º divergent beam, for the spectral
range 270nm to 800nm. The ray tracing model was compared and validated
with the experimental data. Simulation results showed an equivalent
performance for SWIR1 and SWIR3 spectral bands. The Critical Design
Review (CDR) was successfully achieved, and SUSI is currently being
assembled. This work will present the development of the instrument,
details on the tests developed to evaluate its performance, and the
experimental results of the upcoming test campaign.
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Title: The Results of an Era of Teacher Professional Development at
McDonald Observatory
Authors: Finkelstein, K. D.; Hemenway, M. K.; Preston, S.; Wetzel,
M.; Meyer, J.; Rood, M.
2014ASPC..483..369F Altcode:
During the past decade, McDonald Observatory has been developing
and refining its Teacher Professional Development Workshops, many
of which have been supported by NASA. Metrics include attendance,
perceived knowledge gain, and readiness to apply what was learned in the
classroom. Evaluations show impact through the classroom application at
five to six months after the workshops and through consistently high
positive workshop results. This paper will show that a) our Teacher
Professional Development Workshops are consistently well attended, b)
the workshops improve teachers' confidence and their understanding of
concepts, c) teachers enjoy <P />unique interactions with astronomers
and engineers, d) teachers appreciate hands-on and inquiry-based
activities that are modeled and tied to state and national standards,
and e) many teachers experience using the activities in their classrooms
with good results.
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Title: COMET C/2013 UQ4 (Catalina)
Authors: Gajdos, S.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Abe,
H.; Rinner, C.; Kugel, F.; Klotz, A.; Soulier, J. -F.; Diepvens,
A.; Hills, K.; Sandwich, P.; Feliciano, C.; Meyer, J.; Sanford, B.;
Tilley, S. M.; Cranford, D. G., Jr.; Sato, H.; Masek, M.; Honkova,
K.; Jurysek, J.; Lozano, J.; Novichonok, A.; Prystavski, T.; Hudin,
L.; Vintdevara, C.; Paul, N.; Bryssinck, E.; Lister, T.; Maury, A.;
Bosch, J. -G.; Noel, T.; Williams, G. V.
2014MPEC....M...70G Altcode:
No abstract at ADS
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Title: 2014 GT34
Authors: Buzzi, L.; Hill, R. E.; Sanders, R. J.; Christensen, E. J.;
Gibbs, A. R.; Grauer, A. D.; Johnson, J. A.; Kowalski, R. A.; Larson,
S. M.; Shelly, F. C.; Linder, T.; Holmes, R.; Baker, K.; Schwartz,
M.; Holvorcem, P. R.; Meyer, J.; Cranford, D. G., Jr.; Hug, G.; Losse,
F.; Lister, T.
2014MPEC....G...40B Altcode:
No abstract at ADS
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Title: Observations and Orbits of Comets
Authors: Kostov, A.; Enikova, P.; Latev, G.; Kadota, K.; Abe, H.;
Seki, T.; Stevens, B. L.; Baransky, A.; McMillan, R. S.; Mastaler,
R. S. McMillan R. A.; Bressi, T. H.; Kowalski, R. A.; Hill, R. E.;
Boattini, A.; Christensen, E. J.; Gibbs, A. R.; Grauer, A. D.; Johnson,
J. A.; Larson, S. M.; Shelly, F. C.; Durig, D. T.; Satterwhite, K. L.;
Ikari, Y.; Schwartz, M.; Holvorcem, P. R.; Castellano, J.; Storey, D.;
Salto, J. L.; Naves, R.; Klotz, A.; Kugel, F.; Caron, J.; Nicolas,
J.; Aymami, J. M.; Linder, J.; Bel, J.; De Queiroz, J.; Audejean,
M.; Bryssinck, E.; Soulier, J. -F.; Diepvens, A.; Zilch, T.; Gerke,
V.; Plaksa, S.; Prystavski, T.; Gao, X.; Hui, M. -T.; Lindner, P.;
Gaitan, J.; Jahn, J.; Nevski, V.; Ohshima, Y.; Hills, K.; Takahashi,
T.; Primak, N.; Schultz, A.; Goggia, T.; Willman, M.; Veres, P.;
Felber, T.; Cox, P.; Dadighat, M.; Feliciano, C.; Meyer, J.; Ilas,
P.; Evans, A. J.; Paul, N.; Smith, K.; Cranford, D. G., Jr.; Dymock,
R.; Lau, P. S.; Elenin, L.; Savanevych, V.; Bryukhovetskiy, A.; Haugh,
T.; Hug, G.; Sherrod, P. C.; Sherrod, L. P.; Bell, C.; Waszczak, A.;
Masek, M.; Cerny, J.; Ebr, J.; Prouza, M.; Kubanek, P.; Jelinek, M.;
Honkova, K.; Jurysek, J.; Conte, M.; Lozano, J.; Fernandez, F.; Martin,
J. L.; Limon, F.; Gonzalez, J.; Lobao, P.; Hernandez, J. F.; Garcia,
F.; Birtwhistle, P.; Loudeche, A.; Boussier, H.; Arnold, L.; Furgoni,
R.; Benishek, V.; Hudin, L.; Stoian, A. M.; Oey, J.; Camilleri, P.;
Williams, H.; Maury, A.; F Soulier, J.; G Bosch, J.; Soldan A., F. C.
2013MPEC....W...01K Altcode:
No abstract at ADS
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Title: Observations and Orbits of Comets
Authors: Trondal, O.; Kadota, K.; Abe, H.; Seki, T.; Shimomoto,
S.; Sato, H.; Szakats, R.; Sarneczky, K.; Masi, G.; Nocentini,
F.; Masi, U.; Osterhage, K. -F.; Jung, M.; Bill, H.; Baransky, A.;
Vorontseva, A.; Zaets, Z.; Bressi, T. H.; McMillan, R. S.; Scotti,
J. V.; Riabokin, M.; Larsen, J. A.; Johnson, J. A.; Kowalski, R. A.;
Hill, R. E.; Boattini, A.; Christensen, E. J.; Gibbs, A. R.; Grauer,
A. D.; Larson, S. M.; Shelly, F. C.; Hug, G.; Ikari, Y.; Schwartz,
M.; Holvorcem, P. R.; Castellano, J.; Vidal, J. R.; James, N.; Storey,
D.; Salto, J. L.; Naves, R.; Jaeger, M.; Vollmann, W.; Prosperi, E.;
Prosperi, S.; Klotz, A.; Kugel, F.; Caron, J.; Nicolas, J.; Overhaus,
C.; Montoro, L.; Bosch, J. M.; Olivera, R.; Audejean, M.; Bryssinck,
E.; Soulier, J. F.; Diepvens, A.; Hegedus, T.; Borkovits, T.; Biro,
I. B.; Szing, A.; Csorgei, T.; Aledo, J.; Dangl, G.; Gaitan, J.;
Tremosa, L.; Zhao, H. B.; Li, B.; Xia, Y.; Zhaori, G.; Hong, R. Q.;
Hu, L. F.; Lu, H.; Hills, K.; Takahashi, T.; Herald, D.; Primak, N.;
Schultz, A.; Goggia, T.; Willman, M.; Veres, P.; Cox, P.; Dadighat, M.;
Feliciano, C.; Meyer, J.; Ilas, P.; Cranford, D. G., Jr.; McKeegan,
G.; Jung, C.; Bacci, P.; Paul, N.; Sherrod, P. C.; Sherrod, L. P.;
Waszczak, A.; Masek, M.; Cerny, J.; Ebr, J.; Prouza, M.; Kubanek, P.;
Jelinek, M.; Honkova, K.; Jurysek, J.; Conte, M.; Lozano, J.; Martin,
J. L.; Luis Martin Velasco, J.; Buczynski, D.; Carrillo, J.; Limon,
F.; Gonzalez, J.; Carreno, A.; Piqueras, J.; Hernandez, J. F.; Garcia,
F.; Ory, M.; Mas, V.; Fornas, G.; Fletcher, J.; Furgoni, R.; Favero,
G.; Benishek, V.; Benishek, B.; Hudin, L.; Vintdevara, C.; Dumitriu,
A.; Liu, J.; Maury, A.; F Soulier, J.; G Bosch, J.; Jacques, C.;
Pimentel, E.; Barros, J.; Williams, G. V.
2013MPEC....U...73T Altcode:
No abstract at ADS
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Title: Comet P/2011 CR42 (catalina)
Authors: Vales, J.; Ligustri, R.; Waszczak, A.; Boattini, A.;
Hill, R. E.; Kowalski, R. A.; Grauer, A. D.; Ahern, J. D.; Beshore,
E. C.; Garradd, G. J.; Gibbs, A. R.; Larson, S. M.; McNaught, R. H.;
Bezpalko, M.; Torres, D.; Kracke, R.; Spitz, G.; Kistler, J.; Stuart,
J.; Scruggs, S.; Durig, D. T.; Liu, H.; Pietschnig, M.; Zhao, H. B.;
Yao, J. S.; Zhaori, G. T.; Lu, H.; Wang, M.; Hong, R. Q.; Hu, L. F.;
Xia, Y.; Miller, P.; Roche, P.; Tripp, A.; Miles, R.; Holmes, R.;
Foglia, S.; Buzzi, L.; Vorobjov, T.; Lister, T.; Ryan, W. H.; Ryan,
E. V.; Guido, E.; Sostero, G.; Tigges, F.; Meyer, J.; Juenger, C.;
Peters, J. P.; Becker, M.; Bill, H.; Baroni, S.; Concari, P.; Galli,
G.; Tombelli, M.; Chestnov, D.; Novichonok, A.; Ofek, E. O.; Ory,
M.; Sanchez, S.; Nomen, J.; Stoss, R.; Hurtado, M.; Yeung, W. K. Y.;
Jaume, J. A.; Sato, H.; Williams, G. V.
2013MPEC....U...85V Altcode:
No abstract at ADS
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Title: Observations and Orbits of Comets
Authors: Lehky, M.; Bacci, P.; Tesi, L.; Fagioli, G.; Cernis, K.;
Selevicius, H.; Boyle, R. P.; Zdanavicius, J.; Kadota, K.; Seki, T.;
Masi, G.; Nocentini, F.; Masi, U.; Boattini, A.; Christensen, E. J.;
Gibbs, A. R.; Grauer, A. D.; Hill, R. E.; Johnson, J. A.; Kowalski,
R. A.; Larson, S. M.; Shelly, F. C.; Ikari, Y.; Vidal, J. R.; Storey,
D.; Salto, J. L.; Naves, R.; Cozzi, E.; Denzau, H.; Kugel, F.; Caron,
J.; Klotz, A.; Bosch, J. M.; Olivera, R.; Bryssinck, E.; Diepvens, A.;
Gao, X.; Hui, M. -T.; Dangl, G.; Gaitan, J.; Ohshima, Y.; Takahashi,
T.; Herald, D.; Miles, R.; Primak, N.; Schultz, A.; Goggia, T.;
Willman, M.; Veres, P.; Campuzano, F.; Cox, P.; Meyer, J.; Feliciano,
C.; Greg, D.; Cranford, D. G., Jr.; Smith, K.; Ilas, P.; Dadighat,
M.; Yanamandra, P.; Thaluang, T.; Suzuki, M.; Novichonok, A.; Guido,
E.; Howes, N.; Nicolini, M.; Sato, H.; Sherrod, P. C.; Lozano, J.;
Martin, J. L.; Carreno, A.; Piqueras, J.; Hernandez, J. F.; Garcia,
F.; Mas, V.; Brines, P.; Benishek, V.; Hudin, L.; Armstrong, J. D.;
Micheli, M.; Maury, A.; Soulier, J. F.; Williams, G. V.
2013MPEC....U...17L Altcode:
No abstract at ADS
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Title: Nuclear response for the Skyrme effective interaction with
zero-range tensor terms. III. Neutron matter and neutrino propagation
Authors: Pastore, A.; Martini, M.; Buridon, V.; Davesne, D.; Bennaceur,
K.; Meyer, J.
2012PhRvC..86d4308P Altcode: 2012arXiv1207.4006P
The formalism of the linear response for the Skyrme energy density
functional including tensor terms derived in Refs. for nuclear matter
is applied here to the case of pure neutron matter. As in Ref. we
present analytical results for the response function in all channels,
the Landau parameters, and the odd-power sum rules. Special emphasis is
given to the inverse energy weighted sum rule because it can be used to
detect nonphysical instabilities. Typical examples are discussed and
numerical results shown. Moreover, as a direct application, neutrino
propagation in neutron matter is investigated through its neutrino
mean-free path at zero temperature. This quantity turns out to be very
sensitive to the tensor terms of the Skyrme energy density functional.
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Title: A Teacher Professional Development Program on Comets
Authors: Hemenway, M. K.; Cochran, A.; Meyer, J.; Green, W.; Rood, M.
2012ASPC..457..253H Altcode:
Various elements of a workshop centered on the EPOXI flyby of comet
103P/Hartley 2 were combined to meet several goals: participation
in the Galileo Teacher Training Program, relation to a NASA mission,
introduction to the Year of the Solar System, and continuing relations
with teachers to pass current information on to their communities. The
program elements include a residential workshop for teachers at McDonald
Observatory, a short workshop at the Texas state science teachers'
meeting, evaluation, and continuing electronic communication with
participants. Evaluation results indicate the workshop successfully
prepared teachers to implement activities and disseminate the new
information with their students and their colleagues.
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Title: Precession of the Lunar Core
Authors: Meyer, J.; Wisdom, J.
2011epsc.conf..170M Altcode: 2011DPS....43..170M
Goldreich [3] showed that a lunar core of low viscosity would not
precess with the mantle. We show that this is also the case for much of
lunar history. But when the Moon was close to the Earth the Moon's core
was forced to follow closely the precessing mantle, in that the rotation
axis of the core remained nearly aligned with the symmetry axis of the
mantle. The transition from locked to unlocked core precession occurred
between 26.0 and 29.0 Earth radii, thus it is likely that the lunar
core did not follow the mantle during the Cassini transition. Dwyer
and Stevenson [1] suggested that the lunar dynamo needs mechanical
stirring to power it. The stirring is caused by the lack of locked
precession of the lunar core. So, we do not expect a lunar dynamo
powered by mechanical stirring when the Moon was closer to the Earth
than 26.0 to 29.0 Earth radii. A lunar dynamo powered by mechanical
stirring might have been strongest near the Cassini transition.
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Title: Dynamic Elastic Tides
Authors: Meyer, J.; Wisdom, J.
2011epsc.conf..171M Altcode: 2011DPS....43..171M
We present a formulation for solid body tides that includes the
frequency dependence of the tidal dissipation in a self-consistent,
modular way. We derive general expressions for tidal heating and
rate of change of semimajor axis and eccentricity. We then specify
a Kelvin-Voigt rheology, which corresponds to a constant time lag
tidal model commonly used in the literature. We verify that our model
produces the classical expressions and present several new expansions
to high eccentricity.
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Title: Minor Planet Observations [H10 Tzec Maun Observatory, Mayhill]
Authors: Wodaski, R.; Chestnov, D.; Novichonok, A.; Linder, J.;
Baroni, S.; Buzzi, L.; Concari, P.; Foglia, S.; Galli, G.; Tombelli,
M.; Camilleri, P.; Bill, H.; Tigges, F.; Meyer, J.; Juenger, C.;
Peters, J. P.; Becker, M.; Kryachko, T. V.; Korotkiy, S.; Martin,
A.; Schwab, E.; Plaksa, S.; Lebedeva, T.; Bryssinck, E.; Sostero, G.;
Guido, E.; Karge, S.; Kryachko, T.; Tirsky, I.; Mark, K.; Nikiforov, V.
2011MPC..74225...1W Altcode:
No abstract at ADS
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Title: Observations and Orbits of Comets
Authors: Honkova, M.; Tichy, M.; Ticha, J.; Kocer, M.; Jaeger, M.;
Prosperi, E.; Prosperi, S.; Vollmann, W.; Buzzi, L.; Almendros,
I.; Naves, R.; Campas, M.; Reina, E.; Ligustri, R.; Beltrame, P.;
Bressi, T. H.; Asami, A.; Hashimoto, N.; Nishiyama, K.; Okumura, S.;
Sakamoto, T.; Urakawa, S.; Kadota, K.; Wakuda, S.; Endate, K.; Kuli,
Z.; Sarneczky, K.; Kurti, S.; Donato, L.; Gonano, V.; Baransky, A.;
Baransky, B.; Baranska, O.; McMillan, R. S.; Hill, R. E.; Kowalski,
R. A.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.;
Gibbs, A. R.; Grauer, A. D.; Larson, S. M.; McNaught, R. H.; Blythe,
M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.;
Valdivia, A.; Salvo, R.; Roland, S.; Bruzzone, S.; Tancredi, G.;
Martinez, M.; Durig, D. T.; Stinson, J. W. L.; Ikari, Y.; Dupouy, P.;
Kocher, P.; Rinner, C.; Kugel, F.; Camarasa, J.; Lopesino, J.; Bosch,
J. M.; Haeusler, B.; Bryssinck, E.; Sachot, G.; Soulier, J.; de Groote,
B.; Zilch, T.; Ohshima, Y.; Hills, K.; Yusa, T.; Baroni, S.; Concari,
P.; Foglia, S.; Galli, G.; Tombelli, M.; Chestnov, D.; Novichonok, A.;
Dymock, R.; Camilleri, P.; Ryan, W. H.; Ryan, E. V.; Sato, H.; Suzuki,
M.; Guido, E.; Sostero, G.; Meyer, J.; Juenger, C.; Becker, M.; Bill,
H.; Shurpakov, S.; Elenin, L.; Sherrod, P. C.; Bell, C.; Limon, F.;
Gonzalez, J.; Baez, J.; Garcia, F.; Ruiz, J. M.; Williams, G. V.
2011MPEC....C...16H Altcode:
No abstract at ADS
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Title: Minor Planet Observations [H10 Tzec Maun Observatory, Mayhill]
Authors: Foglia, S.; Galli, G.; Tombelli, M.; Juenger, C.; Becker,
M.; Meyer, J.; Peters, J. P.; Shurpakov, S.; Sachs, J.; Karge, S.;
Baroni, S.; Concari, P.; Lebedeva, T.; Linder, J.; Kryachko, T.;
Mark, K.; Tirsky, I.; Nikiforov, V.; Concari, .
2011MPC..73440...6W Altcode:
No abstract at ADS
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Title: Observations and Orbits of Comets
Authors: Kostov, A.; Bilkina, B.; Mikuz, B.; Jaeger, M.; Prosperi, E.;
Vollmann, W.; Sergeyev, A.; Novichonok, A.; Chestnov, D.; Galli, G.;
Buzzi, L.; Naves, R.; Campas, M.; Reina, E.; Ligustri, R.; Bressi,
T. H.; Wakuda, S.; Sanchez, A.; Donato, L.; Gonano, V.; Guido, E.;
Sostero, G.; Meyer, M.; Baransky, A.; Pasichnyk, P.; Larson, S. M.;
Boattini, A.; Ahern, J. D.; Beshore, E. C.; Garradd, G. J.; Gibbs,
A. R.; Grauer, A. D.; Hill, R. E.; Kowalski, R. A.; McNaught,
R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler,
P.; Mackintosh, R.; Konishi, M.; Salvo, R.; Roland, S.; Bruzzone,
S.; Tancredi, G.; Martinez, M.; Durig, D. T.; Ikari, Y.; Vidal,
J. R.; Dupouy, P.; Baldris, F.; Cortes, E.; Rinner, C.; Kugel, F.;
Trigo-Rodriguez, J. M.; Garrigos Sanchez, A.; Nevski, V.; Camarasa,
J.; Nicolas, J.; Overhaus, C.; Bosch, J. M.; Bryssinck, E.; Sachot,
G.; Diepvens, A.; Zilch, T.; Sugiyama, Y.; Koishikawa, M.; Takahashi,
T.; Concari, P.; Foglia, S.; Tombelli, M.; Camilleri, P.; Ryan, W. H.;
Sato, H.; Suzuki, M.; Juenger, C.; Becker, M.; Meyer, J.; Peters,
J. P.; Bill, H.; Shurpakov, S.; Plaksa, S.; Lebedeva, T.; Elenin, L.;
Bell, C.; Gonzalez, J.; Hernandez, J. F.; Tate, J. R.; Martin, J. J.;
Garcia, F.; Muler, G.; Ruiz, J. M.; Fletcher, J.; Williams, G. V.
2010MPEC....Y...12K Altcode:
No abstract at ADS
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Title: Solidifying the lunar magma ocean: Model results and
geochronology (Invited)
Authors: Elkins-Tanton, L. T.; Burgess, S. D.; Meyer, J.; Wisdom, J.
2009AGUFM.P33D..03E Altcode:
The Moon is posited to have formed by reconsolidation of materials
produced during a giant impact with the Earth early in solar system
evolution. The young Moon appears to have experienced a magma ocean of
some depth, which resulted in the formation of an anorthosite flotation
crust. There is no simple way to reconcile W-Hf results for the age of
Moon formation, U-Pb and Sm-Nd ages of lunar crustal crystallization,
and modeling results for magma ocean solidification. At the beginning
of magma ocean solidification the dense iron- and magnesium-rich phases
crystallizing from the cooling magma are believed to have sunk to the
bottom of the magma ocean. When approximately 80% of the lunar magma
ocean solidified, anorthite began to crystallize and float upward
through the more dense magma ocean liquid; anorthite will continue
to be added to this flotation crust until the last dregs of the
magma ocean solidify. The crystallization times of the anorthite in
the flotation crust, therefore, could span the range from about 80%
solidification to what has been interpreted as the lunar magma ocean
solidification age. Models including convection in the remaining
magma ocean, conduction through the growing anorthosite lid, and
radiation into space indicate that the magma ocean may freeze to the
point of anorthosite formation in less than 104 years, and perhaps as
little as 103 years. After this brief free-surface cooling period the
growth of the anorthosite lid radically slows heat loss, and complete
solidification of the magma ocean will require additional tens of
millions of years. Young anorthosite crustal ages, far younger
than models would predict possible, may be explained by further
investigations into the evolution of the lunar orbit. Tidal heating of
the anorthosite crust as the young Moon experiences a period of high
eccentricity may delay closure of minerals with radiogenic phases;
these late-closing minerals will then yield young ages, though they
originally formed far closer to the lunar origin age. We will present
magma ocean and orbital models, and compare with geochronology.
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Title: Measurements of differential cross sections of
Z/γ<SUP></SUP>+jets+X events in pp¯ collisions at s=1.96 TeV
Authors: Dø Collaboration; Abazov, V. M.; Abbott, B.; Abolins,
M.; Acharya, B. S.; Adams, M.; Adams, T.; Aguilo, E.; Ahsan, M.;
Alexeev, G. D.; Alkhazov, G.; Alton, A.; Alverson, G.; Alves, G. A.;
Ancu, L. S.; Andeen, T.; Anzelc, M. S.; Aoki, M.; Arnoud, Y.; Arov,
M.; Arthaud, M.; Askew, A.; Åsman, B.; Atramentov, O.; Avila, C.;
Backusmayes, J.; Badaud, F.; Bagby, L.; Baldin, B.; Bandurin, D. V.;
Banerjee, P.; Banerjee, S.; Barberis, E.; Barfuss, A. -F.; Bargassa,
P.; Baringer, P.; Barreto, J.; Bartlett, J. F.; Bassler, U.; Bauer, D.;
Beale, S.; Bean, A.; Begalli, M.; Begel, M.; Belanger-Champagne, C.;
Bellantoni, L.; Bellavance, A.; Benitez, J. A.; Beri, S. B.; Bernardi,
G.; Bernhard, R.; Bertram, I.; Besançon, M.; Beuselinck, R.; Bezzubov,
V. A.; Bhat, P. C.; Bhatnagar, V.; Blazey, G.; Blessing, S.; Bloom, K.;
Boehnlein, A.; Boline, D.; Bolton, T. A.; Boos, E. E.; Borissov, G.;
Bose, T.; Brandt, A.; Brock, R.; Brooijmans, G.; Bross, A.; Brown, D.;
Bu, X. B.; Buchanan, N. J.; Buchholz, D.; Buehler, M.; Buescher, V.;
Bunichev, V.; Burdin, S.; Burnett, T. H.; Buszello, C. P.; Calfayan,
P.; Calpas, B.; Calvet, S.; Cammin, J.; Carrasco-Lizarraga, M. A.;
Carrera, E.; Carvalho, W.; Casey, B. C. K.; Castilla-Valdez, H.;
Chakrabarti, S.; Chakraborty, D.; Chan, K. M.; Chandra, A.; Cheu, E.;
Cho, D. K.; Choi, S.; Choudhary, B.; Christofek, L.; Christoudias,
T.; Cihangir, S.; Claes, D.; Clutter, J.; Cooke, M.; Cooper, W. E.;
Corcoran, M.; Couderc, F.; Cousinou, M. -C.; Crépé-Renaudin, S.;
Cuplov, V.; Cutts, D.; Ćwiok, M.; Das, A.; Davies, G.; de, K.;
de Jong, S. J.; de La Cruz-Burelo, E.; Devaughan, K.; Déliot, F.;
Demarteau, M.; Demina, R.; Denisov, D.; Denisov, S. P.; Desai, S.;
Diehl, H. T.; Diesburg, M.; Dominguez, A.; Dorland, T.; Dubey, A.;
Dudko, L. V.; Duflot, L.; Duggan, D.; Duperrin, A.; Dutt, S.; Dyshkant,
A.; Eads, M.; Edmunds, D.; Ellison, J.; Elvira, V. D.; Enari, Y.; Eno,
S.; Ermolov, P.; Escalier, M.; Evans, H.; Evdokimov, A.; Evdokimov,
V. N.; Ferapontov, A. V.; Ferbel, T.; Fiedler, F.; Filthaut, F.;
Fisher, W.; Fisk, H. E.; Fortner, M.; Fox, H.; Fu, S.; Fuess, S.;
Gadfort, T.; Galea, C. F.; Garcia-Bellido, A.; Gavrilov, V.; Gay,
P.; Geist, W.; Geng, W.; Gerber, C. E.; Gershtein, Y.; Gillberg, D.;
Ginther, G.; Gómez, B.; Goussiou, A.; Grannis, P. D.; Greder, S.;
Greenlee, H.; Greenwood, Z. D.; Gregores, E. M.; Grenier, G.; Gris,
Ph.; Grivaz, J. -F.; Grohsjean, A.; Grünendahl, S.; Grünewald,
M. W.; Guo, F.; Guo, J.; Gutierrez, G.; Gutierrez, P.; Haas, A.;
Hadley, N. J.; Haefner, P.; Hagopian, S.; Haley, J.; Hall, I.; Hall,
R. E.; Han, L.; Harder, K.; Harel, A.; Hauptman, J. M.; Hays, J.;
Hebbeker, T.; Hedin, D.; Hegeman, J. G.; Heinson, A. P.; Heintz,
U.; Hensel, C.; Herner, K.; Hesketh, G.; Hildreth, M. D.; Hirosky,
R.; Hoang, T.; Hobbs, J. D.; Hoeneisen, B.; Hohlfeld, M.; Hossain,
S.; Houben, P.; Hu, Y.; Hubacek, Z.; Huske, N.; Hynek, V.; Iashvili,
I.; Illingworth, R.; Ito, A. S.; Jabeen, S.; Jaffré, M.; Jain, S.;
Jakobs, K.; Jamin, D.; Jarvis, C.; Jesik, R.; Johns, K.; Johnson, C.;
Johnson, M.; Johnston, D.; Jonckheere, A.; Jonsson, P.; Juste, A.;
Kajfasz, E.; Karmanov, D.; Kasper, P. A.; Katsanos, I.; Kaushik, V.;
Kehoe, R.; Kermiche, S.; Khalatyan, N.; Khanov, A.; Kharchilava, A.;
Kharzheev, Y. N.; Khatidze, D.; Kim, T. J.; Kirby, M. H.; Kirsch, M.;
Klima, B.; Kohli, J. M.; Konrath, J. -P.; Kozelov, A. V.; Kraus, J.;
Kuhl, T.; Kumar, A.; Kupco, A.; Kurča, T.; Kuzmin, V. A.; Kvita, J.;
Lacroix, F.; Lam, D.; Lammers, S.; Landsberg, G.; Lebrun, P.; Lee,
W. M.; Leflat, A.; Lellouch, J.; Li, J.; Li, L.; Li, Q. Z.; Lietti,
S. M.; Lim, J. K.; Lincoln, D.; Linnemann, J.; Lipaev, V. V.; Lipton,
R.; Liu, Y.; Liu, Z.; Lobodenko, A.; Lokajicek, M.; Love, P.; Lubatti,
H. J.; Luna-Garcia, R.; Lyon, A. L.; Maciel, A. K. A.; Mackin, D.;
Mättig, P.; Magerkurth, A.; Mal, P. K.; Malbouisson, H. B.; Malik,
S.; Malyshev, V. L.; Maravin, Y.; Martin, B.; McCarthy, R.; McGivern,
C. L.; Meijer, M. M.; Melnitchouk, A.; Mendoza, L.; Mercadante,
P. G.; Merkin, M.; Merritt, K. W.; Meyer, A.; Meyer, J.; Mitrevski,
J.; Mommsen, R. K.; Mondal, N. K.; Moore, R. W.; Moulik, T.; Muanza,
G. S.; Mulhearn, M.; Mundal, O.; Mundim, L.; Nagy, E.; Naimuddin, M.;
Narain, M.; Neal, H. A.; Negret, J. P.; Neustroev, P.; Nilsen, H.;
Nogima, H.; Novaes, S. F.; Nunnemann, T.; O'Neil, D. C.; Obrant, G.;
Ochando, C.; Onoprienko, D.; Orduna, J.; Oshima, N.; Osman, N.; Osta,
J.; Otec, R.; Otero Y Garzón, G. J.; Owen, M.; Padilla, M.; Padley,
P.; Pangilinan, M.; Parashar, N.; Park, S. -J.; Park, S. K.; Parsons,
J.; Partridge, R.; Parua, N.; Patwa, A.; Pawloski, G.; Penning,
B.; Perfilov, M.; Peters, K.; Peters, Y.; Pétroff, P.; Piegaia, R.;
Piper, J.; Pleier, M. -A.; Podesta-Lerma, P. L. M.; Podstavkov, V. M.;
Pogorelov, Y.; Pol, M. -E.; Polozov, P.; Popov, A. V.; Potter, C.;
da Silva, W. L. Prado; Protopopescu, S.; Qian, J.; Quadt, A.; Quinn,
B.; Rakitine, A.; Rangel, M. S.; Ranjan, K.; Ratoff, P. N.; Renkel,
P.; Rich, P.; Rijssenbeek, M.; Ripp-Baudot, I.; Rizatdinova, F.;
Robinson, S.; Rodrigues, R. F.; Rominsky, M.; Royon, C.; Rubinov, P.;
Ruchti, R.; Safronov, G.; Sajot, G.; Sánchez-Hernández, A.; Sanders,
M. P.; Sanghi, B.; Savage, G.; Sawyer, L.; Scanlon, T.; Schaile, D.;
Schamberger, R. D.; Scheglov, Y.; Schellman, H.; Schliephake, T.;
Schlobohm, S.; Schwanenberger, C.; Schwienhorst, R.; Sekaric, J.;
Severini, H.; Shabalina, E.; Shamim, M.; Shary, V.; Shchukin, A. A.;
Shivpuri, R. K.; Siccardi, V.; Simak, V.; Sirotenko, V.; Skubic,
P.; Slattery, P.; Smirnov, D.; Snow, G. R.; Snow, J.; Snyder, S.;
Söldner-Rembold, S.; Sonnenschein, L.; Sopczak, A.; Sosebee, M.;
Soustruznik, K.; Spurlock, B.; Stark, J.; Stolin, V.; Stoyanova,
D. A.; Strandberg, J.; Strandberg, S.; Strang, M. A.; Strauss, E.;
Strauss, M.; Ströhmer, R.; Strom, D.; Stutte, L.; Sumowidagdo, S.;
Svoisky, P.; Takahashi, M.; Tanasijczuk, A.; Taylor, W.; Tiller, B.;
Tissandier, F.; Titov, M.; Tokmenin, V. V.; Torchiani, I.; Tsybychev,
D.; Tuchming, B.; Tully, C.; Tuts, P. M.; Unalan, R.; Uvarov, L.;
Uvarov, S.; Uzunyan, S.; Vachon, B.; van den Berg, P. J.; van Kooten,
R.; van Leeuwen, W. M.; Varelas, N.; Varnes, E. W.; Vasilyev, I. A.;
Verdier, P.; Vertogradov, L. S.; Verzocchi, M.; Vilanova, D.; Vint,
P.; Vokac, P.; Voutilainen, M.; Wagner, R.; Wahl, H. D.; Wang,
M. H. L. S.; Warchol, J.; Watts, G.; Wayne, M.; Weber, G.; Weber,
M.; Welty-Rieger, L.; Wenger, A.; Wetstein, M.; White, A.; Wicke,
D.; Williams, M. R. J.; Wilson, G. W.; Wimpenny, S. J.; Wobisch, M.;
Wood, D. R.; Wyatt, T. R.; Xie, Y.; Xu, C.; Yacoob, S.; Yamada, R.;
Yang, W. -C.; Yasuda, T.; Yatsunenko, Y. A.; Ye, Z.; Yin, H.; Yip,
K.; Yoo, H. D.; Youn, S. W.; Yu, J.; Zeitnitz, C.; Zelitch, S.; Zhao,
T.; Zhou, B.; Zhu, J.; Zielinski, M.; Zieminska, D.; Zivkovic, L.;
Zutshi, V.; Zverev, E. G.
2009PhLB..678...45D Altcode: 2009PhLB..678...45A; 2009arXiv0903.1748D
We present cross section measurements for Z/γ<SUP></SUP>+jets+X
production, differential in the transverse momenta of the three leading
jets. The data sample was collected with the DØ detector at the
Fermilab Tevatron pp¯ collider at a center-of-mass energy of 1.96 TeV
and corresponds to an integrated luminosity of 1 fb<SUP></SUP>. Leading
and next-to-leading order perturbative QCD predictions are compared
with the measurements, and agreement is found within the theoretical
and experimental uncertainties. We also make comparisons with
the predictions of four event generators. Two parton-shower-based
generators show significant shape and normalization differences with
respect to the data. In contrast, two generators combining tree-level
matrix elements with a parton shower give a reasonable description
of the shapes observed in data, but the predicted normalizations show
significant differences with respect to the data, reflecting large scale
uncertainties. For specific choices of scales, the normalizations for
either generator can be made to agree with the measurements.
---------------------------------------------------------
Title: Publisher's Note: Majoron emission in muon and tau decays
revisited [Phys. Rev. D 79, 055023 (2009)]
Authors: Hirsch, M.; Vicente, A.; Meyer, J.; Porod, W.
2009PhRvD..79g9901H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Phoenix Student Interns Program: Active Research on Mars
Authors: Bowman, C. D. D.; Camacho, J.; Dorsch, W.; Hurd, D.; Meyer,
J.; Overton, J.; Stocco, K.; Young, N.
2008LPI....39.1796B Altcode:
In the Phoenix Student Interns Program, high school students and
teachers from around the U.S. work with Phoenix Mars Mission scientists
and engineers to do the work associated with exploration and discovery
on Mars in summer 2008.
---------------------------------------------------------
Title: Probing Halo Substructure With Rr Lryae From Multi-epoch
Sdss Data.
Authors: Fraser, Oliver J.; Grammer, S. H.; Morgan, D. P.; Welch,
A. Z.; Bullock, E. W.; Huehnerhoff, J.; Kalif, M. L.; Maas, R. W.;
Muhs, E.; Ule, N. M.; Hilton, E. J.; Meyer, J.; Laws, C.; Sesar, B.;
Ivezic, Z.
2007AAS...211.6009F Altcode: 2007BAAS...39..844F
We used RR Lyrae candidates from Sesar et. al. (2007) to investigate
probable over-densities in the Galactic Halo. Candidate RR Lyrae were
selected using multi-epoch SDSS-I observations as stars that vary
more than 0.05 mag (rms) in the SDSS r and g bands, and that have RR
Lyrea colors as described in Ivezic et. al. (2005). The candidates
found using this technique reveal several previously unknown clumps
or over-densities of RR Lryae in the Galactic Halo. The follow-up
photometry obtained at Manastash Ridge Observatory of 40 stars in
three of these over-densities typically includes 20-30 points per
light curve. We find that two-thirds of our sample of 40 stars has
light curves consistent with RR Lyrae, and that the over-densities
likely indicate substructure in the Galactic Halo.
---------------------------------------------------------
Title: Sciamachy Solar Occultation: Ozone and NO<SUB>2</SUB>
Profiles 2003-2005
Authors: Bramstedt, K.; Bracher, A.; Meyer, J.; et al.
2006ESASP.628E..57B Altcode: 2006atsc.confE..57B
No abstract at ADS
---------------------------------------------------------
Title: Numerical and Analytical Model of an Electrodynamic Dust
Shield for Solar Panels on Mars
Authors: Chen, A.; Meyer, J.; Carlos, C. I.; Linell, B.; Buhler,
C. R.; Clements, S.; Mazumder, M. K.
2006LPI....37.1873C Altcode:
Analytical and numerical calculations are presented for a multi-phase
Voltage and Electric Field over the electrodynamic dust shield parallel
electrodes under Mars environment.
---------------------------------------------------------
Title: Geophysical validation of NO2 profiles from SCIAMACHY lunar
occultation measurements
Authors: Amekudzi, L. K.; Bracher, A.; Bramstedt, K.; Meyer, J.;
von Savigny, C.; Bovensmann, H.; Burrows, J. P.
2006cosp...36.2417A Altcode: 2006cosp.meet.2417A
Vertical profiles of stratospheric NO2 have been retrieved from
lunar transmission spectra measured by Scanning Imaging Absorption
Spectrometer for Atmospheric Chartography SCIAMACHY These measurements
were taken over the high Southern latitude of 60-90 degrees during
the period of March to June 2003 and January to June 2004 To assess
the accuracy of the retrieved NO2 profiles the SCIAMACHY nighttime NO2
profiles were compared with daytime NO2 profiles measured by Halogen
Occultation Experiment HALOE Polar Ozone and Aerosol Measurement
POAM-III and the Stratospheric Aerosol and Gas Experiment SAGE-II using
photo chemical correction model The outcome of these validations are
presented in this paper
---------------------------------------------------------
Title: Lunar occultation with SCIAMACHY: First retrieval results
Authors: Amekudzi, L. K.; Bracher, A.; Meyer, J.; Rozanov, A.;
Bovensmann, H.; Burrows, J. P.
2005AdSpR..36..906A Altcode:
Scanning imaging absorption spectrometer for atmospheric chartography
(SCIAMACHY) is a moderate resolution imaging spectrometer on board the
environmental satellite (ENVISAT) launched in March 2002. SCIAMACHY
has eight channels, covering a spectral range from 240 to 2380 nm
and observes the Earth's atmosphere in nadir, limb, and occultation
geometries. From SCIAMACHY lunar occultation measurements, nighttime
vertical profiles of O <SUB>3</SUB> and NO <SUB>2</SUB> have been
retrieved over the southern hemisphere (60°-90°S) using the optimal
estimation method. The first preliminary validation of retrieved
O <SUB>3</SUB> profiles with halogen occultation experiment and
comparisons with stratospheric aerosol and gas experiment III (SAGE
III), and Michelson interferometer for passive atmospheric sounding
(MIPAS) O <SUB>3</SUB> profiles were carried out. In addition,
the retrieved NO <SUB>2</SUB> profiles were compared to SAGE III
and MIPAS results. The results of these preliminary validation and
comparisons give confidence that reasonable scientific data products
(trace gas profiles) can be derived from SCIAMACHY spectroscopic lunar
occultation data.
---------------------------------------------------------
Title: Exploring The Saturn System In The Thermal Infrared: The
Composite Infrared Spectrometer
Authors: Flasar, F. M.; Kunde, V. G.; Abbas, M. M.; Achterberg, R. K.;
Ade, P.; Barucci, A.; Bézard, B.; Bjoraker, G. L.; Brasunas, J. C.;
Calcutt, S.; Carlson, R.; Césarsky, C. J.; Conrath, B. J.; Coradini,
A.; Courtin, R.; Coustenis, A.; Edberg, S.; Edgington, S.; Ferrari,
C.; Fouchet, T.; Gautier, D.; Gierasch, P. J.; Grossman, K.; Irwin,
P.; Jennings, D. E.; Lellouch, E.; Mamoutkine, A. A.; Marten, A.;
Meyer, J. P.; Nixon, C. A.; Orton, G. S.; Owen, T. C.; Pearl, J. C.;
Prangé, R.; Raulin, F.; Read, P. L.; Romani, P. N.; Samuelson, R. E.;
Segura, M. E.; Showalter, M. R.; Simon-Miller, A. A.; Smith, M. D.;
Spencer, J. R.; Spilker, L. J.; Taylor, F. W.
2004SSRv..115..169F Altcode:
The Composite Infrared Spectrometer (CIRS) is a remote-sensing
Fourier Transform Spectrometer (FTS) on the Cassini orbiter that
measures thermal radiation over two decades in wavenumber, from 10
to 1400 cm<SUP>- 1</SUP> (1 mm to 7μ m), with a spectral resolution
that can be set from 0.5 to 15.5 cm<SUP>- 1</SUP>. The far infrared
portion of the spectrum (10 600 cm<SUP>- 1</SUP>) is measured with
a polarizing interferometer having thermopile detectors with a
common 4-mrad field of view (FOV). The middle infrared portion
is measured with a traditional Michelson interferometer having
two focal planes (600 1100 cm<SUP>- 1</SUP>, 1100 1400 cm<SUP>-
1</SUP>). Each focal plane is composed of a 1× 10 array of HgCdTe
detectors, each detector having a 0.3-mrad FOV. CIRS observations
will provide three-dimensional maps of temperature, gas composition,
and aerosols/condensates of the atmospheres of Titan and Saturn
with good vertical and horizontal resolution, from deep in their
tropospheres to high in their mesospheres. CIRS’s ability to observe
atmospheres in the limb-viewing mode (in addition to nadir) offers
the opportunity to provide accurate and highly resolved vertical
profiles of these atmospheric variables. The ability to observe with
high-spectral resolution should facilitate the identification of
new constituents. CIRS will also map the thermal and compositional
properties of the surfaces of Saturn’s icy satellites. It will
similarly map Saturn’s rings, characterizing their dynamical and
spatial structure and constraining theories of their formation and
evolution. The combination of broad spectral range, programmable
spectral resolution, the small detector fields of view, and an orbiting
spacecraft platform will allow CIRS to observe the Saturnian system
in the thermal infrared at a level of detail not previously achieved.
---------------------------------------------------------
Title: Lunar occultation with SCIAMACHY: First retrieval results
Authors: Amekudzi, L. K.; Bracher, A.; Meyer, J.; Rozanov, A.;
Sinnhuber, M.; Bovensmann, H.; Burrows, J. P.
2004cosp...35.1973A Altcode: 2004cosp.meet.1973A
SCIAMACHY (SCanning Imaging Absorption spectroMeter for Atmospheric
CHartographY) is a moderate resolution spectrometer onboard ENVISAT
(Environmental Satellite) launched in March, 2002. The SCIAMACHY
spectrometer has 8 overlapping channels covering a spectral range
of 240--2380 nm and observes sunlight transmitted through and
scattered by the Earth's atmosphere in nadir, limb and occultation
geometries. From lunar occultation measurements above the southern
hemisphere the height resolved profiles of O<SUB>3</SUB>, NO<SUB>2</SUB>
and NO<SUB>3</SUB> were retrieved using SCIAMACHY lunar occultation
level 0 data. Tranmittance spectra showing the absorption features
of O<SUB>3</SUB>, NO<SUB>2</SUB> and NO<SUB>3</SUB> were obtained
by spectral fitting of differential structures of the transmitted
radiation through the atmosphere.The retrieval algorithm is based
on the Optimal Estimation Method. Our retrieved O<SUB>3</SUB>, and
NO<SUB>2</SUB> profiles were compared to SAGE III results. Nighttime
NO<SUB>3</SUB> results were compared with 1-d model results as first
step of validation. The quality of the current profile products will
be discussed.
---------------------------------------------------------
Title: Towards O <SUB>3</SUB> and NO <SUB>2</SUB> vertical profile
retrieval from SCIAMACHY solar occultation measurements: first results
Authors: Meyer, J.; Schlesier, A.; Rozanov, A.; Bovensmann, H.;
Burrows, J.
2004AdSpR..34..744M Altcode:
SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY
(SCIAMACHY) is a space-borne instrument, which measures in the UV-Vis-IR
range in nadir, limb, and occultation geometry. It has successfully
been launched onboard ENVISAT (ENVIronmental SATellite) on March
1 2002. During the six month commissioning phase of ENVISAT, first
test retrievals using uncalibrated Level 0 data were performed. We
retrieved O <SUB>3</SUB> and NO <SUB>2</SUB> height resolved profiles
with considerable accuracy and compared them to POAM III and SAGE
III results. Tangent heights were calculated by O <SUB>2</SUB>
and CO <SUB>2</SUB> retrievals. The retrieval is based on the
optimal estimation method. The spectral fits of O <SUB>3</SUB> and NO
<SUB>2</SUB> absorption spectra were analysed and the fit residues show
remaining spectral inhomogeneities of the solar disk and instrumental
features. An algorithm has been developed to minimise the impact of
the solar inhomogeneities.
---------------------------------------------------------
Title: Exploring the Saturn System in the Thermal Infrared: The
Composite Infrared Spectrometer
Authors: Flasar, F. M.; Kunde, V. G.; Abbas, M. M.; Achterberg, R. K.;
Ade, P.; Barucci, A.; Bézard, B.; Bjoraker, G. L.; Brasunas, J. C.;
Calcutt, S.; Carlson, R.; Césarsky, C. J.; Conrath, B. J.; Coradini,
A.; Courtin, R.; Coustenis, A.; Edberg, S.; Edgington, S.; Ferrari,
C.; Fouchet, T.; Gautier, D.; Gierasch, P. J.; Grossman, K.; Irwin,
P.; Jennings, D. E.; Lellouch, E.; Mamoutkine, A. A.; Marten, A.;
Meyer, J. P.; Nixon, C. A.; Orton, G. S.; Owen, T. C.; Pearl, J. C.;
Prangé, R.; Raulin, F.; Read, P. L.; Romani, P. N.; Samuelson, R. E.;
Segura, M. E.; Showalter, M. R.; Simon-Miller, A. A.; Smith, M. D.;
Spencer, J. R.; Spilker, L. J.; Taylor, F. W.
2004chm..book..169F Altcode:
The Composite Infrared Spectrometer (CIRS) is a remote-sensing
Fourier Transform Spectrometer (FTS) on the Cassini orbiter that
measures thermal radiation over two decades in wavenumber, from 10
to 1400 cm<SUP>-1</SUP> (1 mm to 7 µm), with a spectral resolution
that can be set from 0.5 to 15.5 cm<SUP>-1</SUP>. The far infrared
portion of the spectrum (10-600 cm<SUP>-1</SUP>) is measured with a
polarizing interferometer having thermopile detectors with a common
4-mrad field of view (FOV). The middle infrared portion is measured
with a traditional Michelson interferometer having two focal planes
(600-1100 cm<SUP>-1</SUP>, 1100-1400 cm<SUP>-1</SUP>). Each focal
plane is composed of a 1 × 10 array of HgCdTe detectors, each detector
having a 0.3-mrad FOV. CIRS observations will provide three-dimensional
maps of temperature, gas composition, and aerosols/condensates of the
atmospheres of Titan and Saturn with good vertical and horizontal
resolution, from deep in their tropospheres to high in their
mesospheres. CIRS's ability to observe atmospheres in the limb-viewing
mode (in addition to nadir) offers the opportunity to provide
accurate and highly resolved vertical profiles of these atmospheric
variables. The ability to observe with high-spectral resolution should
facilitate the identification of new constituents. CIRS will also map
the thermal and compositional properties of the surfaces of Saturn's
icy satellites. It will similarly map Saturn's rings, characterizing
their dynamical and spatial structure and constraining theories of
their formation and evolution. The combination of broad spectral range,
programmable spectral resolution, the small detector fields of view,
and an orbiting spacecraft platform will allow CIRS to observe the
Saturnian system in the thermal infrared at a level of detail not
previously achieved.
---------------------------------------------------------
Title: Development of an Online Virtual Laboratory for Introductory
Astronomy
Authors: Parete-Koon, S.; Lingerfelt, E. J.; Dessieux, L.; Kincaid,
R. W.; Browne, M.; Meyer, J.; Guidry, M. W.; Lee, K. M.; Siedell,
C. M.; McMahon, E.
2003AAS...202.1005P Altcode: 2003BAAS...35..712P
We describe a comprehensive set of twenty virtual laboratories for
introductory astronomy that have been developed at the University
of Tennessee and the University of Nebraska for use in lab-based
sequences. These laboratories are fully web-deliverable and built using
Flash MX Actionscript and Java technology, and employ professional
interface design. The virtual laboratories are designed to be usable
in either a supervised laboratory setting, where the student has direct
help available from a teaching assistant, or in a distance environment,
where the student must rely more extensively on intrinsic help available
within the vlabs themselves. Modular design of the vlabs permits an
instructor to tailor varying degrees of difficulty by including or
omitting individual sections of each lab. This flexibility permits
the vlabs to also be used as supplemental interactive material
for non-laboratory courses. A central goal of each laboratory is
inclusion of at least one section requiring the student to interact
with real data available from the Web. We shall discuss both the
technical implementation of these laboratories and our experience
with using them with students. <P />*Managed by UT-Battelle, LLC,
for the U.S. Department of Energy under contract DE-AC05-00OR22725.
---------------------------------------------------------
Title: Solar occultation with SCIAMACHY: First results and validation
Authors: Meyer, J.; Schlesier, A.; Rozanov, A.; Rozanov, V. V.;
Bovensmann, H.; Burrows, J. P.
2003EAEJA.....3798M Altcode:
SCIAMACHY (SCanning Imaging Absorption spectroMeter for Atmospheric
CHartographY) has successfully been launched onboard ENVISAT
(ENVIronmental SATellite) in March 2002. It is measuring
scattered, reflected, and direct radiation in the UV-Vis-IR
range in three different viewing geometries (nadir, limb, and
solar/lunar occultation). The focus of this presentation is on
first solar occultation results. The retrieval algorithm is based
on the optimal estimation method. It is specialised on the spectral
fitting of differential structures of radiation transmitted through
the atmosphere. Height resolved profiles of O_3, NO_2, O_2, and CO_2
were derived from the occultation data. O_3 and NO_2 as natural first
scientific goals can be retrieved with considerable accuracy. First
results of the validation activities will be shown. Retrieved profiles
of O_2 and CO_2 are used to improve the information about tangent
heights as they are well mixed constituents of the atmosphere and can
also be calculated from pressure and temperature profiles.
---------------------------------------------------------
Title: SCIAMACHY on ENVISAT: In-Flight Performance and First Results
Authors: Bovensmann, H.; Ahlers, B.; Buchwitz, M.; Frerick, J.; Goede,
A.; Kaiser, J.; Lichtenberg, G.; Meyer, J.; Noel, S.; Rozanov, A.;
Rozanov, V.; Schlesier, A.; Skupin, J.; Wuttke, M.; Burrows, J.
2002cosp...34E2589B Altcode: 2002cosp.meetE2589B
On 1st of March 2002 ENVISAT with SCIAMACHY on-board was launched
successfully in a sun-synchronous polar orbit. SCIAMACHY is a passive
remote sensing instrument, which measures solar back scattered
and reflected light from the atmosphere in nadir and limb viewing
geometries during the majority of an orbit. In addition solar and lunar
occultation measurements will be performed regularly. Measurements are
made with moderate spectral resolution (0.2 - 1.5 nm) simultaneously in
eight spectral channels covering the spectral region between 220 and
2400 nm. After a few weeks of out gassing SCIAMACHY was switched on
successfully and a complex procedure starts to check out the instrument
in orbit and tune it to the optimum in-flight performance. First
solar and atmospheric spectra were already taken at the begin of April
2002. The talk will present an overview about the status of SCIAMACHY
in orbit and will give some preliminary results on trace gas retrievals
with an outlook on the availability of first operational and scientific
data products.
---------------------------------------------------------
Title: SCIAMACHY Solar Occultation Observations: Retrieval Methods
and First Results
Authors: Meyer, J.; Schlesier, A.; Rozanov, A.; Rozanov, V.;
Bovensmann, H.; Burrows, J.
2002cosp...34E2534M Altcode: 2002cosp.meetE2534M
SCIAMACHY (SCanning Imaging Absorption spectroMeter for Atmospheric
CHartographY) has been launched onboard ENVISAT (Environmental
Satellite) on March 1, 2002. The spectrometer is observing scattered,
reflected, and direct radiation in the UV-Vis-IR range in three
different viewing geometries: nadir, limb, and occultation. This
presentation focuses on the evaluation of the solar occultation
measurements. The retrieval of trace gas profiles is fairly simple in
occultation viewing geometry as only attenuation of direct irradiation
has to be taken into account. In principle, this is done by applying the
Lambert-Beer-Law of Extinction to the observed transmissions. Critical
to the retrieval of atmospheric profiles is the ability to find the
true path of the observed radiation through the atmosphere and to
determine the exact pointing of SCIAMACHY's field of view on the solar
disk. Once this has successfully been mapped to the corresponding
reference measurement above the atmosphere, transmission spectra can
be obtained by simple division. We will present retrieval methods
as applied to SCIAMACHY occultation observations together with first
retrieved trace gas profiles.
---------------------------------------------------------
Title: Joint Cassini, Galileo and Ground-Based Infrared Observations
of Jupiter's Atmosphere
Authors: Orton, G.; Fisher, B.; Barnard, L.; Edberg, S.; Martin, T.;
Spilker, L.; Tamppari, L.; Ustinov, E.; Harrington, J.; Conrath, B.;
Gierasch, P.; Deming, D.; Flasar, F. M.; Kunde, V.; Achterberg, R.;
Bjoraker, G.; Brasunas, J.; Carlson, R.; Jennings, D.; Nixon, C.;
Pearl, J.; Romani, P.; Samuelson, R.; Simon-Miller, A.; Smith, M.;
Abbas, M.; Ade, P.; Barucci, A.; Bezard, B.; Courtin, R.; Coustenis,
A.; Gautier, D.; Lellouch, E.; Marten, A.; Calcutt, S.; Irwin, P.;
Read, P.; Taylor, F.; Owen, T.; Cesarsky, C.; Ferrari, C.; Meyer,
J. P.; Travis, L.; Coradini, A.; Prangee, R.; Grossman, K.; Spencer, J.
2001DPS....33.0905O Altcode: 2001BAAS...33.1035O
During the simultanous Galileo and Cassini encounter with Jupiter
in December, 2000, and January, 2001, data on its atmosphere were
obtained simultaneously by (1) Galileo's Photopolarimeter-Radiometer
(PPR) at 27 microns, (2) Cassini's Composite Infrared Spectrometer
(CIRS) between 7 and 16 microns, and (3) ground-based imaging from the
NASA IRTF between 5 and 24 microns. These data sets mapped temperature
structure, minor and trace constituent abundances and the NH<SUB>3</SUB>
condensate cloud field. Features observed by the three sets of data
included the Great Red Spot (GRS), the merged white oval “BA”,
and 5-micron hot spots. In addition, the IRTF data provided (a)
contextual information for planetary-scale and regional phenomena,
such as thermal waves and polar airmasses, as well as (b) a study of
the evolution of various phenomena. The GRS remains the coldest feature
in Jupiter's upper troposphere at temperate or equatorial latitudes,
and it is consistent with an upwelling cyclonic vortex. A warm region
remains semi-permanently associated with it to the south. Little
thermal variability is detectable that can be associated with the
5-micron hot spots. Jupiter exhibits seasonal variability in its
stratosphere, and the “quasiquadrennial oscillation” of the last 12
years dominates the time variability of the stratosphere. Greater than
normal abundances of NH<SUB>3</SUB> gas are associated with regions of
substantial cloudiness. The meridional variability of zonally averaged
para-H<SUB>2</SUB> abundances is similar to that observed by Voyager
IRIS at Jupiter; it is more abundant in the Great Red Spot than in
surrouding regions. Implications of these and other observations will
be discussed. This work was supported by NASA grants to JPL, GSFC and
Cornell, as well as the Galileo and Cassini projects.
---------------------------------------------------------
Title: Cassini CIRS Observations in the Jovian Environment
Authors: Flasar, F. M.; Kunde, V. G.; Abbas, M.; Achterberg, R. K.;
Ade, P.; Barucci, A.; Bézard, B.; Bjoraker, G.; Brasunas, J.;
Calcutt, S.; Carlson, R.; Césarsky, C.; Conrath, B. J.; Coradini,
A.; Courtin, R.; Coustenis, A.; Edberg, S.; Ferrari, C.; Gautier, D.;
Gierasch, P. J.; Grossman, K.; Irwin, P.; Jennings, D. E.; Lellouch,
E.; Marten, A.; Meyer, J. P.; Nixon, C.; Orton, G.; Owen, T.; Pearl,
J. C.; Prangé, R.; Raulin, F.; Read, P.; Romani, P. N.; Samuelson,
R. E.; Simon-Miller, A.; Smith, M.; Spilker, L.; Taylor, F.
2001AGUSM...P51A05F Altcode:
The Composite Infrared Spectrometer (CIRS) consists of two
interferometers, one polarizing, the other a conventional Michaelson
interferometer, which together provide broad spectral coverage from
10 cm<SUP>-1</SUP> to 1400 cm<SUP>-1</SUP> (1 mm to 7 μ m), at a
resolution as high as 0.5 cm<SUP>-1</SUP>. CIRS functions both as a
thermometer and assayer of the target body, retrieving both thermal
structure and composition. The Cassini spacecraft's 140-R<SUB>J</SUB>
flyby past Jupiter has enabled CIRS to observe Jupiter, its
satellites, and its ring for six months with a spatial resolution up
to 2.5<SUP>o</SUP> of jovian latitude at the subspacecraft point. This
talk will include early results on Jupiter's atmospheric composition
obtained from the relatively unexplored spectral region >50 μm,
Jupiter's planetary-scale temperature field, and the compositional
anomalies and temperatures associated with its auroral hot spots.
---------------------------------------------------------
Title: Overview of the High Resolution Fly's Eye Cosmic Ray
Observatory
Authors: Archbold, Gregory C.; Abassi, R.; Abu-Zayyad, T.; Belov, K.;
Cao, Z.; Christopherson, S.; Everett, A.; Gray, R.; Jones, B. F.; Jui,
C. C. H.; Kieda, D. B.; Kim, K.; Loh, E. C.; Martens, K.; Matthews,
J. N.; Meyer, J.; Moore, S. A.; Moosman, A.; Morrison, P.; Mumford,
R.; Reil, K.; Riehle, R.; Smith, J. D.; Sokolsky, P.; Springer,
R. W.; Stokes, B.; Thomas, S. B.; Wienke, L.; Vanderveen, T.; Yates,
A.; Bellido, J.; Dawson, B. R.; Clay, R. W.; Simpson, K.; Boyer,
J.; Ho, Y.; Knapp, B.; Lee, W.; Mannel, E. J.; Seman, M.; Song, C.;
Westerhoff, S.; Zhang, X.; Belz, J.; Dieterle, B. D.; Martin, G.;
Matthews, J. A. J.; Riley, S.; Bergman, D.; Hanlon, W.; Thompson,
G.; Manago, N.; Sasaki, M.; Sasano, M.; Teshima, M.; Chikawa, M.
2000APS..4CF.DA002A Altcode:
The High Resolution (HiRes) Fly's Eye cosmic ray observatory is used
to detect and study the highest energy particles. The HiRes detector
utilizes the atmosphere as a calorimeter to perform measurements of the
energies of the primary cosmic rays as well as determine the energy
spectrum and composition of cosmic rays and search for anisotropy in
arrival direction. A description of the Air Flourescence detection
technique and the associated physics along with an overview of the
HiRes detector will be presented.
---------------------------------------------------------
Title: Nuclear surface and curvature properties for SLy Skyrme forces
and nuclei in the inner neutron-star crust.
Authors: Douchin, F.; Haensel, P.; Meyer, J.
2000NuPhA.665..419D Altcode:
The properties of nuclear surface, including lowest order curvature
terms, below and above the neutron drip point, are studied
using recent SLy Skyrme models of the effective nucleon-nucleon
interaction. Numerical results are compared with those obtained for
older Skyrme forces, and applied in the compressible liquid drop
model calculations of neutron rich nuclei in the ground state of
neutron-star crust. Five possible types of nuclear structures are
considered, characterized by spherical, cylindrical, and plane nuclear
matter-neutron gas interface.
---------------------------------------------------------
Title: Interpreting the Cosmic Ray Composition
Authors: O'C. Drury, L.; Ellisson, D. C.; Meyer, J. -P.
2000NuPhA.663..843O Altcode: 1999astro.ph..5008D; 1999astro.ph..5008O
Detailed composition measurements can be a very powerful means
of tracing origins, a fact used regularly by forensic scientists
and art historians. One of the main motivating factors for making
detailed observations of cosmic rays was always the hope that a unique
compositional signature could be found which pointed unambiguously
to a particular source. This has proven much harder than expected,
but we have now reached a point where it appears possible to begin to
decipher the information contained in the compositional data; the key,
we have discovered, is to read the data not in isolation, but in the
context provided by our general astronomical knowledge and by recent
developments in shock acceleration theory (Meyer, Drury and Ellison,
1997, 1998; Ellison, Drury and Meyer, 1997). In our view (not, it is
only fair to warn the reader, yet universally accepted) the data show
clearly that the Galactic cosmic ray particles originate predominantly
from the gas and dust of the general interstellar medium.
---------------------------------------------------------
Title: Renormalisation-Group Flow-Equations at Finite Density
Authors: Meyer, J.; Pirner, H. -J.
2000udq..conf..178M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Study of Anisotropy in Arrival Directions in the Highest
Energy Cosmic Rays from High Resolution Fly's Eye Results
Authors: Abu-Zayyad, T.; Archbold, G.; Arisaka, K.; Belov, K.; Belz,
J.; Bergman, D.; Boyer, J.; Cao, Z.; Chen, G.; Clay, R. W.; Dawson,
B. R.; Dieterle, B. D.; Gray, R.; Jones, B.; Jui, C. C. H.; Kieda, D.;
Knapp, B.; Lee, W.; Loh, E. C.; Mannel, E. J.; Martin, G.; Matthews,
J. N.; Matthews, J. A. J.; Meyer, J.; Mumford, R.; Reil, K.; Riley,
S.; Seman, M.; Shaevitz, M.; Smith, J.; Slater, W.; Sokolsky, P.; Song,
C. W.; Stokes, B.; Tessier, T.; Taylor, S. F.; Thomas, S. B.; Thompson,
G.; Wiencke, L.; Vanderveen, T.; Zhang, S.; HIRES Collaboration
1999ICRC....3..296A Altcode: 1999ICRC...26c.296A
We report results on the anisotropy of arrival directions of cosmic
rays with energies greater than 3x1018 . The rst of two High Resolution
Fly's Eye sites began taking data in early 1997. While construction
at the second site continued, the rst site has collected about 20
months of data in monocular mode operation. We examine this data for
dependence on galactic or super-galactic latitude.
---------------------------------------------------------
Title: The Origin of Present Day Cosmic Rays: Fresh SN Ejecta or
Interstellar Medium Material ? I Cosmic Ray Composition and SN
Nucleosynthesis. A Conflict with the Early Galactic Evolution of Be ?
Authors: Meyer, J. P.; Ellison, D. C.
1999astro.ph..5037M Altcode:
The composition of present day cosmic rays (CRs) is inconsistent with a
significant acceleration of SN ejecta material (even with a preferential
acceleration of ejecta grain material). Current CRs must result
mainly from the acceleration of ISM ("solar mix") and circumstellar
(22Ne- and 12C-rich WR wind) gas and grain material. The CR source
composition, indeed, shows no anomaly related to SN nucleosynthesis:
(i) The CR source FeNi/MgSiCa ratios have precisely solar mix
values, while FeNi are mainly synthesized in SN Ia's, and MgSiCa
in SN II's. If CR's originate in SN ejecta, this requires tight
conditions on the acceleration efficiencies of the various SN Ia's
and SN II's. (ii) The non-deficiency of the main-s-process elements,
not made in any SN, relative to all elements made in SNae. (iii)
All CR source isotope ratios are consistent with solar mix (except
for the 22Ne and 12C excesses, WR wind). (iv) The absence of 59Ni in
CRs implies that the time delay between the SN nucleosynthesis and
their acceleration is > 10^5 yr. (v) The physics of SNR's and of CR
shock acceleration implies that the acceleration of interior ejecta
material is comparatively insignificant (Ellison & Meyer, this
volume). Predominant acceleration of current CRs out of superbubble
material also seems implausible. These conclusions regarding current
CRs do not necessarily conflict with the linear evolution of Be/H
in the early Galaxy. With the near absence of heavy elements in the
early Galactic ISM, indeed, the acceleration of even a minute amount
of freshly processed material must have then played a dominant role
for the generation of Be from C and O. The "Be indicator" is blind
to a possibly dominant early Galactic CR component originating in the
ISM then composed of virtually pure H and He.
---------------------------------------------------------
Title: The Origin of Present Day Cosmic Rays: Fresh SN Ejecta or
Interstellar Medium Material ? II Physics of the SNR shock wave
acceleration
Authors: Ellison, D. C.; Meyer, J. P.
1999astro.ph..5038E Altcode:
Assuming that refractory elements in cosmic rays originate in dust
grains, we examine the viability of cosmic ray origin models wherein the
bulk of present day cosmic rays are accelerated out of fresh supernova
ejecta material before it mixes with the average interstellar medium
(ISM). We conclude that the fresh ejecta scenarios that have been
proposed thus far have serious flaws, and are unable to account for
known properties of present day cosmic rays. These flaws include:
(1) the small fraction of ejecta to ISM mass processed by the forward
supernova remnant (SNR) shock; (2) the difficulty fresh ejecta grains
have in reaching the forward shock in isolated SNRs, and the small
expected sputtering yield, especially ahead of the shock, even if grains
do reach the forward shock; (3) the implausibility that fresh ejecta
material can dominate cosmic ray production in diffuse superbubbles;
and (4) the lack of a connection in fresh ejecta models between the
production of cosmic ray refractory and volatile elements. We conclude
that the near linear increase in Be abundance with metallicity observed
in old, halo stars cannot imply that a significant fraction of the
cosmic rays seen today come from fresh supernova ejecta. This conclusion
is supported by the analysis of the present day cosmic ray composition,
as shown in Meyer & Ellison, this volume.
---------------------------------------------------------
Title: The Origin of Present Day Cosmic Rays: Fresh SN Ejecta or
Interstellar Medium Material?
Authors: Ellison, D. C.; Meyer, J. -P.; Drury, L. O'C.
1999AAS...194.2805E Altcode: 1999BAAS...31..865E
Assuming that cosmic ray refractory material originates in dust grains,
we examine the viability of cosmic ray origin models wherein the bulk of
present day cosmic rays are accelerated out of fresh supernova ejecta
material before it mixes with the average interstellar medium. We
conclude that the fresh ejecta scenarios that have been proposed thus
far have serious flaws and are unable to account for known properties
of present day cosmic rays. This implies that the near linear increase
in Be abundance with metallicity observed in old, halo stars cannot
imply that a significant fraction of the cosmic rays seen today come
from fresh supernova ejecta.
---------------------------------------------------------
Title: The Origin of the Present Day Cosmic Rays (I)
Authors: Meyer, Jean-Paul; Ellison, Donald C.
1999ASPC..171..187M Altcode: 1999lcrr.conf..187M
No abstract at ADS
---------------------------------------------------------
Title: The Origin of the Present Day Cosmic Rays (II)
Authors: Ellison, Donald C.; Meyer, Jean-Paul
1999ASPC..171..207E Altcode: 1999lcrr.conf..207E
No abstract at ADS
---------------------------------------------------------
Title: Interpreting the cosmic ray composition
Authors: Drury, L. O'C.; Meyer, J. P.; Ellison, D. C.
1999tcra.conf..171D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Cosmic Rays From ISM Gas and Dust
Authors: Ellison, D. C.; Meyer, J. -P.; Drury, L. O'C.
1998tx19.confE.624E Altcode:
We show that the cosmic ray composition, with no exceptions, can
be accounted for to within experimental uncertainties if SNR shocks
accelerate ambient ISM material consisting of gas and dust. Standard
and well-tested assumptions for efficient diffusive shock acceleration,
combined with a simple model for the energy losses and sputtering of
the shock accelerated grains, result in an enhancement (relative to
hydrogen) of volatile elements which is an increasing function of
mass, and a net, nearly mass-independent enhancement of refractory
elements. The relatively high abundances of C, O are accounted for
since these elements are partially locked in grains and/or have a
Wolf-Rayet contribution. The high H/He ratio may indicate the role of
weak shocks. Furthermore, our shock accelerated spectra are consistent
with observed spectra below the `knee' if a fairly steep rigidity
dependent escape (i.e., ~R^{0.65}) from the galaxy is assumed.
---------------------------------------------------------
Title: Cosmic Rays From Supernova Remnants: a Brief Description of
the Shock Acceleration of gas and Dust
Authors: Ellison, Donald C.; Drury, Luke O'c.; Meyer, Jean-Paul
1998SSRv...86..203E Altcode:
We summarize our model of galactic cosmic-ray (GCR) origin and
acceleration, wherein a mixture of interstellar and/or circumstellar
gas and dust is accelerated by a supernova remnant (SNR) blast wave. A
detailed analysis of observed GCR abundances (Meyer et al., 1997),
combined with the knowledge that many refractory elements known to
be locked in grains in the interstellar medium (ISM) are abundant
in cosmic rays, has lead us to revive an old suggestion (Epstein,
1980) that charged dust grains can be shock accelerated. Here,
we outline results (presented more completely in Ellison et al.,
1997) from a nonlinear shock model which includes (i) the direct
acceleration of interstellar gas-phase ions, (ii) a simplified model
for the direct acceleration of weakly charged grains to ∼100 keV
amu-1 energies, simultaneously with the acceleration of the gas ions,
(iii) the energy losses of grains colliding with the ambient gas, (iv)
the sputtering of grains, and (v) the simultaneous acceleration of the
sputtered ions to TeV energies. We show that the model produces GCR
source abundance enhancements of the volatile, gas-phase elements,
which are an increasing function of mass, as well as a net, mass
independent, enhancement of the refractory, grain elements over protons,
consistent with cosmic-ray observations. The GCR 22Ne and C excesses
may also be accounted for in terms of the acceleration of 22Ne-C-
enriched pre-SN Wolf-Rayet star wind material surrounding the most
massive supernovae. The O excess seen in cosmic rays probably cannot
be interpreted in terms of W-R star nucleosynthesis, but is easily
accounted for in our model since 15 to 20% of O is trapped in grain
cores and this O will be preferentially accelerated. We have expanded
the parameter range explored in Ellison et al. (1997) to lower shock
speeds and higher maximum cosmic-ray energies and find similar fits
to the H/He ratio and the cosmic-ray source spectra.
---------------------------------------------------------
Title: A Cosmic-ray Composition Controlled by Volatility and a/q
Ratio. SNR Shock Acceleration of gas and Dust
Authors: Meyer, Jean-Paul; Drury, Luke O'c.; Ellison, Donald C.
1998SSRv...86..179M Altcode:
The composition of Galactic Cosmic Ray Sources (GCRS) shows the
following features: (i) an enhancement of the refractory elements
relative to the volatile ones, and (ii) an enhancement of the heavier
volatile elements relative to the lighter ones; this mass dependence
should reflect a mass-to-charge (A/Q) dependence of the acceleration
efficiency; among the refractory elements, there is only a very
weak enhancement of heavier species, or none at all. We consider it
fortuitous that the GCRS composition resembles that of the solar corona,
which is biased according to first ionization potential. In a companion
paper by Ellison et al. (1998, this issue), this GCRS composition
is interpreted in terms of a supernova shock wave acceleration of
interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas
phase and especially dust grain material. These two papers summarize
and complement the content of two papers that recently appeared in
Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).
---------------------------------------------------------
Title: A Skyrme parametrization from subnuclear to neutron star
densitiesPart II. Nuclei far from stabilities
Authors: Chabanat, E.; Bonche, P.; Haensel, P.; Meyer, J.; Schaeffer,
R.
1998NuPhA.635..231C Altcode:
In a first paper Skyrme effective forces were revisited in order to
improve their isospin properties away from the β stability line. In
this paper, these forces are specifically adjusted to reproduce finite
nuclei properties. Spin-orbit terms and center of mass correlations
are analyzed. New Skyrme parametrizations are proposed and some of
their spectroscopic properties are presented, e.g. S<SUB>2n</SUB>,
S<SUB>2p</SUB> and r.m.s. radii for different isotopic and isotonic
series.
---------------------------------------------------------
Title: The Relative Merits of Three Different Power Transmission
Systems for Precision Tracking Space Mechanisms
Authors: Meyer, J.; Petrou, A.
1997ESASP.410..265M Altcode: 1997smt..conf..265M
No abstract at ADS
---------------------------------------------------------
Title: Galactic Cosmic Rays from Supernova Remnants. I. A Cosmic-Ray
Composition Controlled by Volatility and Mass-to-Charge Ratio
Authors: Meyer, Jean-Paul; Drury, Luke O'C.; Ellison, Donald C.
1997ApJ...487..182M Altcode: 1997astro.ph..4267M
We show that the Galactic cosmic-ray source (GCRS) composition is best
described in terms of (1) a general enhancement of the refractory
elements relative to the volatile ones, and (2) among the volatile
elements, an enhancement of the heavier elements relative to the
lighter ones. This mass dependence most likely reflects a mass-to-charge
(A/Q) dependence of the acceleration efficiency; among the refractory
elements, there is no such enhancement of heavier species, or only
a much weaker one. We regard as coincidental the similarity between
the GCRS composition and that of the solar corona, which is biased
according to first ionization potential. In a companion paper,
this GCRS composition is interpreted in terms of an acceleration by
supernova shock waves of interstellar and/or circumstellar (e.g.,
<SUP>22</SUP>Ne-rich Wolf-Rayet wind) gas-phase and, especially,
dust material.
---------------------------------------------------------
Title: Galactic Cosmic Rays from Supernova Remnants. II. Shock
Acceleration of Gas and Dust
Authors: Ellison, Donald C.; Drury, Luke O'C.; Meyer, Jean-Paul
1997ApJ...487..197E Altcode: 1997astro.ph..4293E
We present a quantitative model of Galactic cosmic-ray (GCR) origin and
acceleration, wherein a mixture of interstellar and/or circumstellar
gas and dust is accelerated by a supernova remnant blast wave. The gas
and dust are accelerated simultaneously, but differences in how each
component is treated by the shock leave a distinctive signature, which
we believe exists in the cosmic-ray composition data. A reexamination of
the detailed GCR elemental composition, presented in a companion paper,
has led us to abandon the long-held assumption that GCR abundances are
somehow determined by first ionization potential. Instead, volatility
and mass (presumably mass-to-charge ratio) seem to better organize the
data: among the volatile elements, the abundance enhancements relative
to solar increase with mass (except for the slightly high H/He ratio);
the more refractory elements seem systematically overabundant relative
to the more volatile ones in a quasi-mass-independent fashion. If
this is the case, material locked in grains in the interstellar
medium must be accelerated to cosmic-ray energies more efficiently
than interstellar gas-phase ions. Here we present results from a
nonlinear shock model that includes (1) the direct acceleration of
interstellar gas-phase ions, (2) a simplified model for the direct
acceleration of weakly charged grains to ~100 keV amu<SUP>-1</SUP>
energies, simultaneously with the acceleration of the gas ions,
(3) the energy losses of grains colliding with the ambient gas,
(4) the sputtering of grains, and (5) the simultaneous acceleration
of the sputtered ions to GeV and TeV energies. We show that the
model produces GCR source abundance enhancements of the volatile,
gas-phase elements that are an increasing function of mass, as well
as a net, mass-independent enhancement of the refractory, grain
elements over protons, consistent with cosmic-ray observations. We
also investigate the implications of the slightly high H/He ratio. The
GCR <SUP>22</SUP>Ne excess may also be accounted for in terms of the
acceleration of <SUP>22</SUP>Ne-enriched presupernova Wolf-Rayet star
wind material surrounding the most massive supernovae. We also show
that cosmic-ray source spectra, at least below ~10<SUP>14</SUP> eV,
are well matched by the model.
---------------------------------------------------------
Title: Galactic Cosmic Rays from SNRs: Shock Acceleration of Gas
and Dust
Authors: Ellison, Don; Meyer, Jean-Paul; O'C. Drury, Luke
1997APS..APR.M1202E Altcode:
We present a quantitative model of galactic cosmic ray (GCR) origin
and acceleration, wherein a mixture of interstellar gas and dust is
accelerated by a supernova remnant (SNR) blast wave. The gas and dust
are accelerated simultaneously, but differences in how each component
is treated by the shock leaves a distinctive signature which we believe
exists in the cosmic ray data. We abandon the long held assumption
that GCR abundances are determined by first ionization potential
(FIP). Instead, volatility and mass (presumably mass-to-charge ratio)
seem to better organize the data: among the volatile elements, the
abundance enhancements relative to solar increase with mass; the
refractory elements seem systematically overabundant relative to the
more volatile ones in a quasi-mass-independent fashion. We present
results from a nonlinear shock model which includes the acceleration
of gas-phase ions, the acceleration of weakly charged grains to ~ 100
keV/amu energies, frictional energy losses of grains, the sputtering
of grains, and the simultaneous acceleration of the sputtered ions to
TeV energies. The model produces GCR abundances and spectra consistent
with observations.
---------------------------------------------------------
Title: A Skyrme parametrization from subnuclear to neutron star
densities
Authors: Chabanat, E.; Bonche, P.; Haensel, P.; Meyer, J.; Schaeffer,
R.
1997NuPhA.627..710C Altcode:
Skyrme effective forces are revisited to improve their behavior with
respect to the isospin degree of freedom from the stability line to the
most exotic nuclei that coming experimental facilities will produce. To
achieve the best possible calculation of nuclear properties up to the
neutron drip line, it is proposed to fit the neutron matter equation
of state of the UV14+UVII theoretical model up to high densities to
avoid any collapses or unphysical features of the resulting equation
of state in the Skyrme framework. This last and very severe constraint
on these interactions allows a prospective study of both neutron rich
nuclei and neutron star matter.
---------------------------------------------------------
Title: The Helium Valley: Comparison of Impulsive Solar Flare Ion
Abundances and Gyroresonant Acceleration with Oblique Turbulence in
a Hot Multi-Ion Plasma
Authors: Steinacker, Jürgen; Meyer, Jean-Paul; Steinacker, Adriane;
Reames, Donald V.
1997ApJ...476..403S Altcode:
We present a detailed interpretation of the heavy ion abundance
enhancements observed in impulsive flare energetic particles, in terms
of the conditions for gyroresonant acceleration by moderately oblique
waves in a hot solar coronal plasma. <P />On the basis of a realistic
coronal plasma containing its complete set of minor ions, we analyze
first all parallel wave modes in terms of their dispersion relation,
damping timescale, and condition for gyroresonant acceleration of
thermal ions, as a function of temperature. We identify the “Helium
Valley,” the region in the frequency-wavenumber plane of strong wave
damping by thermal <SUP>4</SUP>He<SUP>+2</SUP> ions, as crucial for
explaining the observed abundances: any ions with charge-to-mass ratio
in the neighborhood of 0.5 cannot be accelerated preferentially,
relative to <SUP>4</SUP>He<SUP>+2</SUP>. <P />Then solving the
dispersion relation equation for oblique waves in a hot e-p-He plasma,
we discuss this general class of waves in terms of polarization and
damping timescale. For waves propagating at moderate angles to the
magnetic field (θ ≉ 90°), our calculations indicate that the first
harmonic n = 1 gyroresonance is dominant, and that the corresponding
He valley narrows down for increasing angle θ. Using this analysis, we
calculate the limits of the He valley and investigate the preferential
gyroresonant acceleration of heavy ions by moderately oblique waves
(θ ≉ 90°) in a solar coronal plasma. Only for nearly perpendicular
waves (θ ~ 90°), are higher order resonances important and regions
of wave damping by interaction with thermal particles vanishingly
narrow in frequency. <P />We estimate the fraction of ions of each
element outside the He valley as a function of temperature and compare
the resulting enhanced abundances with the observed enhancements, for
the case of a spectrum of non-quasi-perpendicular waves, as produced
by a cascading of the general turbulence. The results allow us to
specify the range of possible temperatures for the source plasma of
the accelerated particles to between ~2.4 and ~4.5 × 10<SUP>6</SUP>
K, i.e., comparable to active region (AR), but not to flaring gas,
temperatures. This points to an acceleration of the ions taking place,
either in the AR gas surrounding the flare itself or within the flaring
loop but before it became heated. Constraints are set on the typical
time Δt over which the ions are accelerated preferentially. We
find times between ~5 × 10<SUP>-4</SUP> and ~3 × 10<SUP>-2</SUP>
s (for our nominal plasma with density and field of n<SUB>e</SUB> =
10<SUP>10</SUP> cm<SUP>-3</SUP> and B = 100 G); it could be ~10 times
larger, if the typical conditions in quiescent ARs (n<SUB>e</SUB> ~ 2
× 10<SUP>9</SUP> cm<SUP>-3</SUP> and B ~ 200 G) apply also to the bulk
~3 × 10<SUP>6</SUP> K gas of flaring ARs. We discuss another physical
interpretation of Δt, if wave cascading is effective. Preliminary
calculations have shown that the proposed selective acceleration
mechanism can be applied in underdense (ω<SUB>p</SUB>/Ω<SUB>e</SUB>
< 1) as well as in overdense plasmas (our nominal case), provided
that quasi-perpendicular waves (generated, e.g., by an electron beam)
are not dominant.
---------------------------------------------------------
Title: GCR composition: Volatility or FIP? SNR Shock Acceleration
of Gas and Dust.
Authors: Meyer, J. P.; O'C. Drury, L.; Ellison, D. C.
1997ICRC....4..357M Altcode: 1997ICRC...25d.357M
No abstract at ADS
---------------------------------------------------------
Title: Interstellar dust, shock acceleration and the Galactic Cosmic
Ray Composition
Authors: Ellison, D. C.; O'C. Drury, L.; Meyer, J. -P.
1997ICRC....4..425E Altcode: 1997ICRC...25d.425E
No abstract at ADS
---------------------------------------------------------
Title: Accelerated particle composition in impulsive events: Clues
to the conditions of acceleration
Authors: Meyer, Jean-Paul
1996AIPC..374..461M Altcode: 1996hesp.conf..461M
The heavy element composition anomalies systematically found in the
impulsive, <SUP>3</SUP>He-rich, solar energetic particles events are
reviewed. These anomalies imply, in a quasi-model-independent way,
that the particles are accelerated predominantly out of gases with
temperatures in the ∼2.5 to ∼5 MK range, i.e., typical active
region, not flaring loop, temperatures. Existing models for selective
ion acceleration by plasma waves are briefly overviewed. A specific
model to account for the heavy element enhancements is presented,
in terms of the damping of electromagnetic He cyclotron waves by
interaction with <SUP>4</SUP>He ions, which sets constraints to the
source gas temperature and to the acceptable rate of wave cascading. The
high charge states observed among the energetic particles are discussed.
---------------------------------------------------------
Title: Abundance anomalies in the solar outer atmosphere.
Authors: Meyer, J. P.
1996sube.conf...27M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Coronal Abundance Anomalies
Authors: Meyer, J. -P.
1996ASPC...99..127M Altcode: 1996coab.proc..127M
No abstract at ADS
---------------------------------------------------------
Title: Looking for the FIP Effect in EUV Spectra: Examining the
Solar Case
Authors: Haisch, Bernhard; Saba, Julia L. R.; Meyer, Jean-Paul
1996aeu..conf..511H Altcode: 1996IAUCo.152..511H
No abstract at ADS
---------------------------------------------------------
Title: New Skyrme effective forces for supernovae and neutron
rich nuclei.
Authors: Chabanat, E.; Bonche, P.; Haensel, P.; Meyer, J.; Schaeffer,
R.
1995PhST...56..231C Altcode:
New Skyrme-like effective interactions are proposed suitable for neutron
stars, supernovae and neutron-rich nuclei. The parameters of the force
are adjusted to the properties of the symmetric infinite nuclear matter,
with an additional constraint on the low and high density neutron matter
equation of state. Preliminary Hartree-Fock plus BCS calculations along
series of isotopes are shown. They seem to solve the problem of large
discrepancies observed with other parametrizations.
---------------------------------------------------------
Title: Energetic-Particle Abundances in Impulsive Solar Flare Events
Authors: Reames, D. V.; Meyer, J. P.; von Rosenvinge, T. T.
1994ApJS...90..649R Altcode: 1994IAUCo.142..649R
We report on the abundances of energetic particles from impulsive solar
flares, including those from a survey of 228 He-3 rich events, with
He-3/He-4 is greater than 0.1, observed by the International Sun Earth
Explorer (ISEE) 3 spacecraft from 1978 August through 1991 April. The
rate of occurrence of these events corresponds to approximately 1000
events/yr on the solar disk at solar maximum. Thus the resonant plasma
processes that enhance He-3 and heavy elements are a common occurrence
in impulsive solar flares. To supply the observed fluence of He-3
in large events, the acceleration must be highly efficient and the
source region must be relatively deep in the atmosphere at a density
of more than 10<SUP>10</SUP> atoms/cu cm. He-3/He-4 may decrease in
very large impulsive events because of depletion of He-3 in the source
region. The event-to-event variations in He-3/He-4, H/He-4, e/p, and
Fe/C are uncorrelated in our event sample. Abundances of the elements
show a pattern in which, relative to coronal composition, He-4, C, N,
and O have normal abundance ratios, while Ne, Mg, and Si are enhanced
by a factor approximately 2.5 and Fe by a factor approximately 7. This
pattern suggests that elements are accelerated from a region of the
corona with an electron temperature of approximately 3-5 MK, where
elements in the first group are fully ionized (Q/A = 0.5), those in
the second group have two orbital electrons (Q/A approximately 0.43),
and Fe has Q/A approximately 0.28. Ions with the same gyrofrequency
absorb waves of that frequency and are similarly accelerated and
enhanced. Further stripping may occur after acceleration as the ions
begin to interact with the streaming electrons that generated the
plasma waves.
---------------------------------------------------------
Title: Time-development of proton energy spectra in solar energetic
particle events
Authors: Meyer, J.; Wibberenz, G.; Kallenrode, M. -B.
1993AdSpR..13i.363M Altcode: 1993AdSpR..13..363M
Solar energetic particle events often consist of two components: a
`prompt' component of particles accelerated in the flare or by a coronal
shock, and an `energetic storm particle' component accelerated by an
interplanetary shock. In events observed by two or more spacecraft the
time-development of the proton spectrum, together with the analysis of
the intensity and anisotropy time profiles, allows one to distinguish
between these components.
---------------------------------------------------------
Title: Elemental abundances in active regions, flares and
interplanetary medium
Authors: Meyer, Jean-Paul
1993AdSpR..13i.377M Altcode: 1993AdSpR..13..377M
Not Available <P />Permanent address.
---------------------------------------------------------
Title: Element fractionation at work in the solar atmosphere.
Authors: Meyer, J. -P.
1993oee..conf...26M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Stratospheric H2 O-18 and H2 O-17 measurements from
balloon-borne infrared spectra
Authors: Camy-Peyret, C.; Flaud, J. M.; Karcher, F.; Meyer, J. P.;
Murcray, D.; Murcray, F.; van Allen, J.
1992AnGeo..10..267C Altcode:
Independent balloon-borne observations of H2 O-18 and H2 O-17 isotopes
using solar absorption Fourier transform spectrometry in the strong
6.3 micron band of water vapor are reported. Isotopic enhancement
factors with respect to H2 O-16 of 0.97 +/- 0.06 and 1.16 +/- 0.15
have been found for H2 O-18 and H2 O-17, respectively. These results
confirm previous observations by mid- and far-infrared spectrometry
which show no evidence of significant stratospheric enhancements.
---------------------------------------------------------
Title: Hartree-Fock Description of Superdeformed States
Authors: Dobaczewski, J.; Bonche, P.; Flocard, H.; Heenen, P. H.;
Krieger, S. J.; Meyer, J.; Weiss, M. S.
1992ftna.conf..109D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Element Abundances in Solar <SUP>3</SUP>He-Rich Events
Authors: Reames, D. V.; Cane, H. V.; von Rosenvinge, T. T.; Meyer,
J. -P.
1991ICRC....3..319R Altcode: 1991ICRC...22c.319R; 1991icrc...22....7R
The results of a survey of over 228 (He-3)-rich events, with He-3/H-4
of more than 0.1, observed by the ISEE-3 spacecraft from 1978 August
through 1991 April. In these events the elements above C are enhanced
relative to the corresponding abundances in the corona and the degree
of enhancement increases with Z or A. The flare-to-flare variations
in abundances are different in character from those seen in large
proton events. For example, using Fe/C as a parameter to describe these
variations, the slope of the least-squares fits to ln(X/C) vs ln(Fe/C),
where X is the intensity of N, O, Ne, Mg, Si, or S. Slopes of these
abundance-correlation lines are much steeper for the (He-3)-rich events
than for a sample of 36 large proton events, especially for Ne and
heavier ions. The event-to-event variations for the (He-3)-rich events
distinguish 3 groups of elements, He-O, Ne-S, and Fe. The abundances
of all of the species within each group seem to vary in unison.
---------------------------------------------------------
Title: Diagnostic methods for coronal abundances
Authors: Meyer, Jean-Paul
1991AdSpR..11a.269M Altcode: 1991AdSpR..11..269M
The observation evidence of a definite difference between the
composition of the solar photosphere and that of the entire, bulk
corona is reviewed. The coronal abundances are discussed by comparison
with the photospheric abundances. Coronal abundances from coronal
and transition-region gas spectroscopy, from solar-wind in situ
observations, and from solar-energetic-particle in situ observations
are analyzed. Abundances in the chromosphere and key low-lying solar
features are outlined. Tentative scenarios for a first ionization
potential (FIP)-dependent fractionation between photosphere and corona
are presented for the low and high coronal abundances of hydrogen. It
is concluded that the FIP-bias of the coronal heavy-element composition
is well established comparing to photosphere, but the general abundances
of these heavy elements relative to hydrogen are not clear.
---------------------------------------------------------
Title: Solar Energetic Particle Observations of the 1982 June 3 and
1980 June 21 Gamma-Ray/Neutron Events
Authors: Van Hollebeke, M. A. I.; McDonald, F. B.; Meyer, J. P.
1990ApJS...73..285V Altcode:
The Helios I cosmic-ray observations of the June 3, 1982 and the June
21, 1980 gamma-ray/neutron events are analyzed. The particle intensity
vs time plots for the two events are presented and the time of maximum
energy spectra, and event-integrated energy spectra are examined. The
H-2/H, H-3/H, and He-3/He-4 ratios and the heavy-element compositions
of the two events are described. Both gamma-ray/neutron events are
shown to be He-3-rich and to have heavy element enhancements that are
characteristic of He-3-rich events.
---------------------------------------------------------
Title: The Nitrogen Deficiency Puzzle: An Underestimate of the
<SUP>20</SUP>Ne Production in Wolf-Rayet Stars?
Authors: Prantzos, N.; Meyer, J. -P.; Arnould, M.
1990ICRC....4...51P Altcode: 1990ICRC...21d..51P; 1989ICRC....4...51P
No abstract at ADS
---------------------------------------------------------
Title: Abundance Differences Between Photosphere and Corona: Diffusive
Fractionation Mechanisms in Chromospheric Material
Authors: Meyer, J. -P.; Vauclair, S.
1990ICRC....5..378M Altcode: 1990ICRC...21e.378M
No abstract at ADS
---------------------------------------------------------
Title: Modelling the Earth's geomagnetic field to high degree
and order.
Authors: Schmitz, Dave R.; Meyer, J.; Cain, Joseph C.
1989GeoJI..97..421S Altcode:
The authors present a method for modelling the Earth's magnetic field
to very high degree and order in terms of spherical harmonics. The
method exploits the orthogonality of the spherical functions, using,
in part, the method of Gauss-Legendre quadrature. This method is
compared to a simpler quadrature method (Newton-Cotes). The authors
show that the Gauss-Legendre technique is more accurate in most cases
than Newton-Cotes quadrature, and in all cases, even where the two
give about the same results, that the Gauss-Legendre method is more
efficient in that it requires less data and hence less computation. The
two quadrature methods are applied to sets of radial field data computed
from an n = 29 model which simulate Magsat observations.
---------------------------------------------------------
Title: The Geomagnetic Spectrum For 1980 and Core-Crustal Separation
Authors: Cain, Joseph C.; Wang, Zhigang; Schmitz, Dave R.; Meyer, J.
1989GeoJI..97..443C Altcode:
The spectrum of a high degree spherical harmonic model of the
geomagnetic field is analyzed to compute the constants for the core
and crustal field contributions. Using a noise estimate of 0.091 nT sq
at the mean Magsat radius of 6791 km, the values for the power reduced
to the earth's surface show half the crustal power extrapolated to n =
0 compared with an n = 23 model, and a white noise depth of only 14
km below the mean surface. The core spectrum power is 30 percent less
than previously estimated and becomes flat 80 km below the core-mantle
boundary. The point where the energy density of the core and crustal
components become equal at the earth's surface is n = 14.2.
---------------------------------------------------------
Title: Solar Abundance Variations
Authors: Meyer, J. -P.
1989BAAS...21..832M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Elemental abundances in the interstellar medium ... and
elsewhere
Authors: Meyer, Jean-Paul
1989AIPC..183..245M Altcode: 1989cam..conf..245M
This review on interstellar abundances certainly does not pretend to
be at all systematic or exhaustive. For instance, I will not at all
cover isotopic determinations in the interstellar medium (the very
rich radio data on isotopes in molecules, the UV studies of deuterium,
the more recent γ-ray studies of 26Al). Nor will I, for instance,
discuss the abundance of S, which has been extensively observed in both
HII regions and HI gas. This paper consists rather in the treatment of
selected topics, with a lot of connections with abundance determinations
in other media, such as stars or solar environment. (AIP)
---------------------------------------------------------
Title: COSTEP: A comprehensive suprathermal and energetic particle
analyzer for SOHO
Authors: Kunow, Horst; Fischer, Harald; Green, Guenter; Mueller-Mellin,
Reinhold; Wibberenz, Gerd; Holweger, Hartmut; Evenson, Paul; Meyer,
Jean-Paul; Hasebe, Nabuyuki; von Rosenvinge, Tycho
1988sohi.rept...75K Altcode:
The group of instruments involved in the COSTEP (comprehensive
suprathermal and energetic particle analyzer) project are
described. Three sensors, the LION (low energy ion and electron)
instrument, the MEICA (medium energy ion composition analyzer) and
the EPHIN (electron proton helium instrument) are described. They are
designed to analyze particle emissions from the sun over a wide range
of species (electrons through iron) and energies (60 KeV/particle to
500 MeV/nucleon). The data collected is used in studying solar and
space plasma physics.
---------------------------------------------------------
Title: Everything You Always Wanted to Ask about Local Galactic
Abundances but Were Afraid to Know
Authors: Meyer, J. -P.
1988ode..conf..337M Altcode:
The author first gives an overall view, intended for non-specialists, of
the problems involved in determining a local Galactic (LG) standard of
abundances. He briefly discusses the recently proposed "SEP-derived
photospheric" abundances, and finally gives an updated table of LG
abundances.
---------------------------------------------------------
Title: Cosmic Rays: Material from Coronae of Ordinary Stars and from
He-Burning Zones
Authors: Meyer, J. -P.
1988ode..conf..310M Altcode:
The galactic cosmic ray (GCR) composition seems to tell us that the bulk
of the GCR nuclei were first extracted out of the coronae of ordinary
F to M stars. They were most likely first accelerated to MeV energies
by stellar flares, and later on boosted up to GeV energies by SNR (and
possibly massive star wind) shocks. A small fraction of them (≡2%)
should originate in He-Burning material, plausibly in Wolf-Rayet
stars. All these views might however have to be questioned if the
recent indications of a deficiency of N in GCR sources are confirmed.
---------------------------------------------------------
Title: Measurement and QCD analysis of the photon structure function
F<SUB>2</SUB>(x, Q<SUP>2</SUP>)
Authors: Berger, Ch.; Genzel, H.; Lackas, W.; Pielorz, J.; Raupach,
F.; Wagner, W.; Klovning, A.; Lillestöl, E.; Bürger, J.; Criegee,
L.; Deuter, A.; Ferrarotto, F.; Franke, G.; Gaspero, M.; Gerke, Ch.;
Knies, G.; Lewendel, B.; Meyer, J.; Michelsen, U.; Pape, K. H.;
Stella, B.; Timm, U.; Winter, G. G.; Zachara, M.; Zimmermann, W.;
Bussey, P. J.; Cartwright, S. L.; Dainton, J. B.; Hendry, D.; King,
B. T.; Raine, C.; Scarr, J. M.; Skillicorn, I. O.; Smith, K. M.;
Thomson, J. C.; Achterberg, O.; Blobel, V.; Burkart, D.; Diehlmann,
K.; Feindt, M.; Kapitza, H.; Koppitz, B.; Krüger, M.; Poppe, M.;
Spitzer, H.; van Staa, R.; Chang, C. Y.; Glasser, R. G.; Kellogg,
R. G.; Maxfield, S. J.; Polvado, R. O.; Sechi-Zorn, B.; Skard,
J. A.; Skuja, A.; Tylka, A. J.; Welch, G. E.; Zorn, G. T.; Almeida,
F.; Bäcker, A.; Barreiro, F.; Brandt, S.; Derikum, K.; Grupen, C.;
Meyer, H. J.; Müller, H.; Neumann, B.; Rost, M.; Stupperich, K.;
Zech, G.; Alexander, G.; Bella, G.; Gnat, Y.; Grunhaus, J.; Junge,
H.; Kraski, K.; Maxeiner, C.; Maxeiner, H.; Meyer, H.; Schmidt, D.
1987NuPhB.281..365B Altcode:
We present a measurement of the hadronic structure function
F<SUB>2</SUB><SUP>γ</SUP>(x, Q<SUP>2</SUP>) of the photon in the
Q<SUP>2</SUP> range from 10 to 100 GeV<SUP>2</SUP>. Data were taken
with the PLUTO detector at the e<SUP>+</SUP>e<SUP>-</SUP> storage
ring PETRA. This measurement and previous PLUTO measurements in the
Q<SUP>2</SUP> range of 1.5 to 16 GeV<SUP>2</SUP> are compared with
higher order QCD calculations. The structure function is consistent with
the predicted log Q<SUP>2</SUP> behaviour when charm contributions are
subtracted. The x dependence can be well described for 0.1 < x <
0.9 by the regularization scheme of Antoniadis and Grunberg. Within
their scheme the data yield a value of Λ<SUB>MS</SUB> = 183 + 65/
-40(stat.) + 46/ -36(sys.) MeV for the QCD scale parameter.
---------------------------------------------------------
Title: Cosmic rays: material from coronae of ordinary stars and from
He-burning zones, but not from s-process sites.
Authors: Meyer, Jean-Paul
1986ana..work..393M Altcode:
The galactic cosmic ray (GCR) composition seems to tell us that the bulk
of the GCR nuclei were first extracted out of the coronae of ordinary
F to M stars. They were most likely first accelerated to MeV energies
by stellar flares, and later on boosted up to GeV energies by SNR (and
possibly massive star wind) shocks. A small fraction of them (≡2%)
should originate in He-burning material, plausibly in Wolf-Rayet stars.
---------------------------------------------------------
Title: Beobachtungsergebnisse der Berliner Arbeitsgemeinschaft für
Veränderliche Sterne e.V. (BAV).
Authors: Huebscher, J.; Lichtenknecker, D.; Meyer, J.
1986BAVSM..43.....H Altcode:
This 19th compilation of BAV results contains 523 observed minima and
maxima on 227 variable stars including 3 photoelectric results.
---------------------------------------------------------
Title: Secular variation of magnetic mean energy density at the
source-layer depth
Authors: Meyer, J.
1985PEPI...39..288M Altcode:
The dipole part of the geomagnetic main field loses its predominant role
with the secular variation of mean energy density if the description
is reduced to the depth of the source-layer, about 100 km below the
core-mantle boundary, as revealed from the spatial spectrum of the
field. The magnetic mean energy density at that level is already
balanced if only two more spectrum terms, i.e., the quadrupole and
octupole constituents, are included. The result is in accordance
with the idea of conservation of energy density as inferred from the
variation of the spectrum. It supports the concept of the presently
observed secular variation to be caused primarily by structural changes
of the current system in the source-layer, associated with an exchange
of energy between spherical harmonic constituents of different degrees,
without involving a systematic change of the generation mechanism.
---------------------------------------------------------
Title: Galactic cosmic ray composition
Authors: Meyer, J. P.
1985ICRC....9..141M Altcode: 1985ICRC...19i.141M
An assessment is given of the galactic cosmic ray source (GCRS)
elemental composition and its correlation with first ionization
potential. The isotopic composition of heavy nuclei; spallation cross
sections; energy spectra of primary nuclei; electrons; positrons;
local galactic reference abundances; comparison of solar energetic
particles and solar coronal compositions; the hydrogen; lead; nitrogen;
helium; and germanium deficiency problems; and the excess of elements
are among the topics covered.
---------------------------------------------------------
Title: Diffusion in the Chromosphere, and the Composition of the
Solar Corona and Energetic Particles
Authors: Vauclair, S.; Meyer, J. P.
1985ICRC....4..233V Altcode: 1985ICRC...19d.233V
Composition observations, in the solar photosphere, and in the upper
transition region (TR) and corona imply a change of composition
of the solar atmosphere somewhere between the photosphere and the
upper TR. Heavy elements with first ionization potential (FIP) 9 eV
(high-FIP element) are approx. 4 times less abundant in the TR and
corona than in the photosphere, as compared to both hydrogen and heavy
elements with lower low-FIP elements. A separation is suggested between
neutral and ionized elements in a region where the high-FIP elements
are mostly neutral, and the low-FIP elements ionized. This occurs in
the chromosphere at altitudes above 600 km and below 2000 km above
Photosphere. Whether the diffusion processes can explain the observed
change in composition is investigated.
---------------------------------------------------------
Title: Germanium and Lead: Significant Differences Between Meteoritic
and Photospheric Abundances?
Authors: Grevesse, N.; Meyer, J. P.
1985ICRC....3....5G Altcode: 1985ICRC...19c...5G
The order of the Galactic cosmic ray source (GCRS) composition in terms
of first ionization potential (FIP) was examined. For most elements,
the degree of volatility is (positively) correlated with the value of
the FIP, so that it is not easy to distinguish a correlation of GCRS
abundances anomalies with FIP from a correlation with volatility. Only
a few permit to distinguish between the two kinds of ordering: if
they are depleted relative to refractory metals, volatility must be
relevant, if not, FIP is relevant. Among them Cu and Zn would seem
to favor FIP. Among the best indicators are Ge and Pb. The abundance
anomalies in GCRS are defined relative to a standard which, for
the heavy elements concerned, is commonly taken as C1 Carbonaceous
Chondrites. Photospheric abundances are more directly representative
of the protosolar nebula, and hence of ordinary local galactic (LG)
matter. The Ge and Pb reference abundance determinations in the
Photosphere and in C1 meteorites are examined and their relevance to
the problem with FIP vs. volatility in GCRs is discussed.
---------------------------------------------------------
Title: The baseline composition of solar energetic particles
Authors: Meyer, J. -P.
1985ApJS...57..151M Altcode:
A comprehensive analysis of spacecraft observations obtained to date
for the highly variable heavy element composition of solar energetic
particles, which exhibit the imprint of a pervasive composition
pattern that differs from the photospheric composition by a simple bias
related to the first ionization potential. In each of the observations,
this mass-unbiased baseline composition is seen to be distorted by an
additional bias that is always a monotonic function of mass. This latter
bias varies in amplitude (and even in sign) among the observations
and appears to be related to differences in the A/Z-asterisk ratio
between elements, where Z-asterisk is the mean effective charge.
---------------------------------------------------------
Title: Solar-stellar outer atmospheres and energetic particles,
and galactic cosmic rays
Authors: Meyer, J. -P.
1985ApJS...57..173M Altcode:
The heavy element compositions of the solar corona, solar wind (SW),
solar energetic particles (SEPs), and galactic cosmic ray sources
(GCRSs) all exhibit the same pattern when compared to standard local
galactic composition; the pattern involves an underabundance of
heavy elements with first ionization potential (FIP) greater than
about 9 eV relative to elements with lower FIP by factors of about
4-6. The similar abundance patterns found in SW, SEP, and GCRS
suggest that they were all extracted from solar stellar coronae,
with their compositions reflecting, to first order, that of their
birthplace. GCRSs are presently interpreted in terms of a two-step
acceleration scenario in which most should be MeV-stellar energetic
particles first injected by flares out of the coronae of unevolved,
later-type stars, which were subsequently reaccelerated to high energy
by strong interstellar shock waves.
---------------------------------------------------------
Title: The crustal contribution to the spatial spectra of the
geomagnetic secular variation.
Authors: Meyer, J.; Hufen, J. -H.; Sibert, M.; Hahn, A.
1985JGG....37.1141M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Current function of the geomagnetic main field in the source
layer atthe core/mantle boundary.
Authors: Meyer, J.; Hufen, J. -H.; Siebert, M.
1985JGZG...57...42M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The decrease of the geomagnetic dipole field as part of the
general secular variation.
Authors: Meyer, J.
1985JGG....37..153M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Composition of the Solar Corona, Solar Flare Particles and
Galactic Cosmic Rays
Authors: Meyer, J. P.
1984BAAS...16..512M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Clues to the origin of cosmic rays derived from their source
composition and energy spectra
Authors: Koch-Miramond, L.; Meyer, J. P.
1984AdSpR...4b..79K Altcode: 1984AdSpR...4Q..79K
Cosmic ray composition and energy spectra at source have been recently
obtained with good precision. The bulk of the observations suggests that
cosmic rays originate in unevolved star surface material. Most cosmic
rays should be stellar energetic particles first accelerated by flares
out of the Coronae of F to M stars, that got later on reaccelerated
to high energy by strong interstellar shock waves. The limitations
of this two-step scenario and of the other plausible stellar and
interstellar models are pointed out. <P />The <SUP>22</SUP>Ne and
carbon excesses at cosmic ray source are accounted for if a minor
component (2%) of cosmic rays are made of He-burning material,
plausibly originating in Wolf-Rayet stars. The possible oxygen and
<SUP>25,26</SUP>Mg excesses could be interpreted in the same context,
but not the <SUP>29,30</SUP>Si excess.
---------------------------------------------------------
Title: Measurement of photon structure functions with the PLUTO
detector
Authors: Meyer, J.
1984npp..conf..523M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: What are cosmic rays made of?
Authors: Cesarsky, C. J.; Meyer, J. -P.
1984EN.....15...12C Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Which Types of Stars are the Dominant Cosmic Ray Injectors?
Authors: Meyer, J. P.
1983ICRC....2..323M Altcode: 1983ICRC...18b.323M
No abstract at ADS
---------------------------------------------------------
Title: Two-Stage Acceleration and Propagation at Low Energy
Authors: Meyer, J. P.
1983ICRC....2..322M Altcode: 1983ICRC...18b.322M
No abstract at ADS
---------------------------------------------------------
Title: a Tentative Ordering of all Available Solar Energetic Particles
Abundance Observations II : Discussion and Comparison with Coronal
Abundances
Authors: Meyer, J. P.
1981ICRC....3..149M Altcode: 1981ICRC...17c.149M
No abstract at ADS
---------------------------------------------------------
Title: A comparison of the elemental abundances in the cosmic ray
sources with local galactic and solar energetic particle abundances
Authors: Goret, P.; Engelmann, J. J.; Koch-Miramond, L.; Meyer, J. P.;
Lund, N.; Rasmussen, I. L.; Perron, C.
1981ICRC....9..122G Altcode: 1982ICRC....9..122G; 1981ICRC...17i.122G
No abstract at ADS
---------------------------------------------------------
Title: Interpretation of the elemental abundances measured by the
French-Danish experiment on HEAO-3 - Interstellar propagation and
derivation of source abundances
Authors: Perron, C.; Engelmann, J. J.; Goret, P.; Juliusson, E.;
Koch-Miramond, L.; Meyer, J. P.; Soutoul, A.; Lund, N.; Rasmussen,
I. L.; Westergaard, N.
1981ICRC....9..118P Altcode: 1981ICRC...17i.118P; 1982ICRC....9..118P
No abstract at ADS
---------------------------------------------------------
Title: On Volatility, First Ionization Potential, and s- and r-
Processes
Authors: Meyer, J. P.
1981ICRC....2..281M Altcode: 1981ICRC...17b.281M
The possibility of a correlation between the first ionization potential
and volatility (in that elements of low potential tend to be refractory
and those of high potential volatile) is considered. It is noted that
the apparent correlation between galactic cosmic ray source (GCRS)
elemental abundances and the first ionization potential may in fact
be based on volatility. Attention is given here to compositional
clues which may determine whether volatility or the first ionization
potential is the relevant parameter. The correlation between the first
ionization potential and volatility is examined, and those elements
which do not fit into the correlation are isolated. Attention is also
given to possible ambiguities in interpreting the charge spectrum
beyond Ni that derive from coincidences between regions of change in
the first ionization (and volatility) and the s- and r-process peaks.
---------------------------------------------------------
Title: Comparative Abundances in Solar Energetic Particles and in
Galactic Cosmic-Ray Sources, and the NE22 Anomaly
Authors: Meyer, J. P.
1981ICRC....2..265M Altcode: 1981ICRC...17b.265M
No abstract at ADS
---------------------------------------------------------
Title: Wolf Rayet stars and the origin of the Ne-22 excess in
cosmic rays
Authors: Casse, M.; Paul, J. A.; Meyer, J. P.
1981IAUS...94...35C Altcode:
First order Fermi acceleration at the boundary between supersonic
stellar winds from OB and WR stars and the surrounding interstellar
medium (ISM), combined with continuous injection of low-energy
particles, could influence the bulk energization of the local cosmic
radiation (CR). Selective effects at injection can explain the
difference between CR source composition and the surface composition
of young stars. Selective acceleration effects do not significantly
alter the isotopic proportions of any given heavy element at the CR
source. The abnormal Ne-22/Ne-20 ratio estimated at the CR source
differs from that in the solar system and is probably due to stellar
wind in WR stars blowing nucleosynthetic Ne-22 away from the surface
of the exposed convective core.
---------------------------------------------------------
Title: a Tentative Ordering of all Available Solar Energetic Particles
Abundance Observations i : the Mass Unbiased Baseline
Authors: Meyer, J. P.
1981ICRC....3..145M Altcode: 1981ICRC...17c.145M
No abstract at ADS
---------------------------------------------------------
Title: Origin of the Solar Cosmic Ray Composition
Authors: Meyer, J. -P.; Cassé, M.
1979ICRC....5...76M Altcode: 1979ICRC...16e..76M
No abstract at ADS
---------------------------------------------------------
Title: The Cosmic-Ray Source Composition as a Probe of the
Acceleration Mechanisms
Authors: Cassé, M.; Meyer, J. -P.; Reeves, H.
1979ICRC....2..114C Altcode: 1979ICRC...16b.114C
No abstract at ADS
---------------------------------------------------------
Title: Do we have any Significant Information on the Relative
Abundances of Platinum, Lead and Actinides in Galactic Cosmic Rays ?
Authors: Meyer, J. -P.
1979ICRC....1..374M Altcode: 1979ICRC...16a.374M
No abstract at ADS
---------------------------------------------------------
Title: The significance of the carbonaceous chondrites abundances -
Introductory report
Authors: Meyer, J. -P.
1979LIACo..22..153M Altcode: 1979eiu..conf..153M; 1979eisu.conf..153M
The paper discusses the significance of the carbonaceous chondrite
(CC) elemental abundances in terms of abundances in the primitive
solar nebula. The abundances are considered in terms of: (1) the
possibility of volatile element enrichments and depletions in CC
matrices, (2) the existence of a unique matrix composition among
C1's, C2's, and C3's based on recent observations of CC matrices, (3)
abundance similarities with solar photosphere, and (4) the continuity of
elemental abundances beyond Fe. It was confirmed that the CC abundances
are highly significant for refractory elements, and that C1 abundances
are probably the best guide to the abundances of volatiles. The high
abundances of Li, Be, and B in meteorites compared with sun and stars
may be the evidence for early solar irradiation.
---------------------------------------------------------
Title: Local Galactic Abundances Revisited
Authors: Meyer, J. -P.
1979ICRC....2..115M Altcode: 1979ICRC...16b.115M
No abstract at ADS
---------------------------------------------------------
Title: The sulphur abundance in the solar neighbourhood
Authors: Meyer, J. -P.
1979LIACo..22..465M Altcode: 1979eiu..conf..465M; 1979eisu.conf..465M
The sulfur abundance in the solar neighborhood is determined from
measurements of meteorites, the solar photosphere, the solar corona
and H II regions. In C 1 carbonaceous chondrites, S equals 50 plus
or minus 8 on a scale of Si equal to 100; in C 2's, S equals 21.5
plus or minus 2. In the solar photosphere the abundance deduced for
permitted S I lines and consistent with the forbidden S I lines is
adopted, that is, S equal to 43 plus or minus 15. In the corona,
EUV and X-ray observations yield an S value of 31 within a factor of
2, and a fairly constant S/O ratio, consistent with Orion's value,
of 0.026 plus or minus 0.007, is found for H II regions with oxygen
abundances varying by a factor of 5. Finally, a value of 45 plus or
minus 13 is adopted for S, that is, for the solar system, S/H equals
(1.65 plus or minus 0.5) x 10 to the -5th power.
---------------------------------------------------------
Title: The Cosmic-Ray Source Composition as a Probe of the
Acceleration Mechanisms. I. General
Authors: Meyer, J. -P.; Casse, M.; Reeves, H.
1979ICRC...12..108M Altcode: 1980ICRC...12..108M; 1979ICRC...16l.108M
A comparison is made between cosmic ray source (CRS) and local galactic
(LG) elemental and isotopic compositions with realistic error bars. The
possible roles of nucleosynthesis and atomic processes in shaping the
CRS composition are discussed. It is found that the major fraction of
the CR nuclei should originate in a medium of normal LG composition,
in which atomic selection effects seem to operate on a singly ionized
gas. In addition, the possible origin of the Ne-22 rich component of
galactic cosmic rays are discussed. The only plausible source is the
explosive processing of H-rich envelopes of novae and supernovae.
---------------------------------------------------------
Title: The neon abundance in the solar neighborhood
Authors: Meyer, J. -P.
1979LIACo..22..489M Altcode: 1979eisu.conf..489M; 1979eiu..conf..489M
Ne abundance determinations on a scale of Si set equal to 100 are
presented for the solar corona, solar wind, H II regions and hot
stars. In the solar corona, observations of the Ne/Mg ratio yield Ne
values of approximately 100 to 200 while Ne of 250 to 450 are found
from the Ne/O ratio. A value of 150, within a factor of 2.5, is adopted
for Ne in the solar wind, and with regard to H II regions, a value of
Ne of 320, within a factor of 1.7, is found in our neighborhood. In
addition, a very high degree of homogeneity of the obtained Ne/O ratio
from various observations suggests that the Ne/O ratio is not in error
due to overlooked charge transfer reactions, that the oxygen abundance
in the gas phase of H II regions is affected only to a limited degree
by incorporation into grains, and that oxygen and neon are synthesized
in related phases of nucleosynthesis.
---------------------------------------------------------
Title: The abundance of lithium, beryllium and boron, and the infall
of extragalactic matter in the Galaxy.
Authors: Reeves, H.; Meyer, J. -P.; Beaudet, G.
1979LIACo..22..285R Altcode: 1979eiu..conf..285R; 1979eisu.conf..285R
No abstract at ADS
---------------------------------------------------------
Title: The argon abundance in the solar neighbourhood
Authors: Meyer, J. -P.
1979LIACo..22..477M Altcode: 1979eiu..conf..477M; 1979eisu.conf..477M
Argon abundance determinations from the solar corona, solar wind,
H I gas, H II regions and hot stars are presented. Emphasis is placed
on Ar in the H I gas, for which Ar abundances deduced from Copernicus
observations towards 12 stars are plotted versus the amount of neutral
hydrogen along the line of sight, as well as versus the interstellar
reddening. Column densities of neutral Ar I are considered along with
the saturated and weakly saturated lines of sight; also discussed is an
apparent gradual decrease of the Ar abundance with N(H(n)) and with the
E(B-V) reddening. A value of 9.0, within a factor of 1.7, is adopted
for Ar on a scale of Si equal to 100, that is, Ar/H is equal to 3.3
x 10 to the -6th power, within a factor of 1.7, for the solar system.
---------------------------------------------------------
Title: Cosmic Rays Accompanying the Birth of the Solar System ?
Authors: Meyer, J. -P.; Reeves, H.
1979ICRC....2..121M Altcode: 1979ICRC...16b.121M
No abstract at ADS
---------------------------------------------------------
Title: Cosmic-ray nucleosynthesis and the infall rate of extragalactic
matter in the solar neighborhood.
Authors: Reeves, H.; Meyer, J. -P.
1978ApJ...226..613R Altcode:
An up-to-date discussion of the galactic abundances of lithium,
beryllium, and boron is presented. The observed galactic abundances
of these elements remain surprisingly constant in time, at values
significantly lower than predictions made by conventional models of
closed galactic evolution. This fact suggests that intergalactic
hydrogen may enter our neighborhood. A local infall rate of about
2 solar masses per billion years per sq pc is favored; the rather
large uncertainties in this rate are discussed. The measured ratios
of element and isotope abundances among the light elements suggest
that the average energy spectrum of fast particles in our galactic
neighborhood turns up below 50-100 MeV per nucleon. Such a turnup
implies that two source families for cosmic rays must exist, perhaps
supernovae and ordinary stars. In carbonaceous chondrites, not only
boron, but apparently also beryllium and perhaps even lithium, seem
to be enriched beyond their stellar abundance values. And even after
many years of study, the origin of Li-7 remains uncertain.
---------------------------------------------------------
Title: Cosmic ray nucleosynthesis, big-bang nucleosynthesis and
galactic infall.
Authors: Reeves, H.; Meyer, J. P.
1978sss..meet...D1R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Report on a Future Experiment at the CERN SPS to Study High
Energy Neutrino Interactions Using Counter Techniques
Authors: Meyer, J.
1978neu2.conf..369M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The recurrence tendency of geomagnetic activity during solar
cycle 20.
Authors: Meyer, J.
1978JGZG...44..427M Altcode:
Values of the equivalent recurrence number of geomagnetic activity are
presented for the years 1971-1976. The recurrence tendency variation
is found to be similar to the pattern associated with previous solar
cycles. The recurrence tendency, lowest in the years immediately
following the preceding sunspot minimum to the time of sunspot maximum
(1965-1968), increases in the years after sunspot maximum (1969-1975)
and remains relatively high throughout 1976. The equivalent recurrence
numbers, introduced by Bartels (1960), are related to the stability
of high-speed solar wind streams.
---------------------------------------------------------
Title: Silicon, Sulphur, Argon, Calcium: Puzzling Thoughts on a
Key Quartet
Authors: Casse, M.; Meyer, J. P.
1977ICRC....2..131C Altcode: 1977ICRC...15b.131C; 1978ICRC....2..131C
It is demonstrated that cosmic ray source abundances of silicon,
sulfur, argon and calcium cannot reflect the quasi-equilibrium of
explosive silicon burning at whatever temperature. In particular,
the low abundances of argon and sulfur in the cosmic ray sources rule
out explosive silicon burning as a mechanism to account for cosmic ray
origins. It is also shown that no single abundance of sulfur in the
Galaxy can be consistent with both nucleosynthesis theory as presently
interpreted and the production of cosmic ray sources.
---------------------------------------------------------
Title: Realistic Uncertainties on Galactic Abundances and Significance
of the Cosmic Ray Source Composition
Authors: Meyer, J. P.; Reeves, H.
1977ICRC....2..137M Altcode: 1978ICRC....2..137M; 1977ICRC...15b.137M
A compilation of galactic elemental abundances with realistic error
estimates is presented and compared with cosmic ray abundances in order
to determine the composition of the galactic cosmic ray source. Galactic
abundances were determined from the compositions of meteorites, the
solar photosphere and corona, the solar wind and interstellar and
stellar matter; the agreement among the various sources is generally
found to be good. Cosmic ray abundances are found to lie with the error
bounds of the calculated galactic N/O and Pb/Pt ratios, indicating
no significant depletions of N or Pb in galactic cosmic ray sources,
however a serious depletion of S has been detected.
---------------------------------------------------------
Title: Cosmic Ray Propagation: Energy-Dependence of Leakage Mean
Path Length
Authors: Fontes, P.; Meyer, J. -P.; Perron, C.
1977ICRC....2..234F Altcode: 1977ICRC...15b.234F; 1978ICRC....2..234F
Propagation calculations making use of the latest experimental nuclear
cross-sections, have been carried out in an attempt to account for
the cosmic ray chemical abundances and their variations as a function
of energy. A survey of the available cosmic ray data has been made,
and these data are consistently corrected for interactions in the
atmosphere. Secondary-to-primary ratios, selected on the basis of their
significance, can be accounted for either by a continuous decrease of
the leakage mean path length with energy or by two distinct propagation
regimes, one below about 5 GeV/n, the other between 20 and 100 GeV/n,
with a transition region in-between.
---------------------------------------------------------
Title: Chlorine 36 and the Cosmic Ray Escape Lifetime. Present Status
Authors: Meyer, J. P.; Casse, M.; Goret, P.
1977ICRC....2..213M Altcode: 1978ICRC....2..213M; 1977ICRC...15b.213M
A lower limit for cosmic ray escape time is proposed on the basis of
recent observations of Cl in cosmic rays, proton- and alpha-induced
cross sections, an interstellar propagation model, and assumptions
concerning source composition. By comparing the Cl abundance to that
of other secondary nuclei rather than to that of Fe, dependence on the
interstellar propagation model can be reduced. It is assumed that no
Cl is accelerated in the sources. The observed Cl abundance in cosmic
rays suggests a cosmic ray escape time larger than about 10 million
years. In addition, revised estimates of spallation cross sections in
air are presented for atmospheric corrections.
---------------------------------------------------------
Title: Light Elements Production by Galactic Cosmic Rays-the State
of Affairs
Authors: Reeves, H.; Meyer, J. P.
1977ICRC....2...54R Altcode: 1978ICRC....2...54R; 1977ICRC...15b..54R
Recent B and Be abundance determinations in meteorites and stars,
including the sun, are used together with previous measurements to
select a set of abundances in various astrophysical environments for
the three light elements Li, Be, and B. Particular care is taken in
the evaluation of the associated uncertainties. Production of Li, Be,
and B by spallation reactions induced by observed high-energy galactic
cosmic rays is considered. It is suggested that the observed galactic
cosmic rays plus a tail of low-energy particles having a power-law
injection spectrum with an exponent of at least 4 can produce the
isotopes Li-6, Be-9, B-10, and B-11 in agreement with the observations
---------------------------------------------------------
Title: Pathlength Distribution and Source Composition of Cosmic Ray
Nuclei. (Abstract)
Authors: Meneguzzi, M.; Cesarsky, C. J.; Meyer, J. P.
1975ICRC....2..652M Altcode: 1975ICRC...14..652M
No abstract at ADS
---------------------------------------------------------
Title: Isotopic Analysis by Slowing-Down Cerenkov-Cerenkov Method
Authors: Meyer, J. P.; Gaulier, F.
1975ICRC....9.3199M Altcode: 1975ICRC...14.3199M
No abstract at ADS
---------------------------------------------------------
Title: Galactic light isotopes: significance of present observations.
Authors: Meyer, J. P.
1975ICRC....2..554M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Isotopic analysis by the Cerenkov-Cerenkov slowing-down method
Authors: Meyer, J. P.
1975rgcr.conf...71M Altcode: 1975ESRO..109...71M; 1975rgcr.rept...71M
The performance of a large-scale Cerenkov-Cerenkov slowing-down setup
for isotope analysis in the 1 to 2 GeV/n region is analyzed. Such a
setup should permit isotope analysis of all nuclei between neon and
nickel with rms mass errors less than 0.5 amu and less than 1 amu over,
respectively, approximately 250MeV/n and approximately 500MeV/n wide
energy ranges. The background associated with the very high rate of
nuclear interactions in the instrument (75%) should be eliminated by
a triple redundancy in the charge measurement. These estimates are
based largely on experience gained from Danish-French balloon flights
and from runs at the Berkeley bevatron.
---------------------------------------------------------
Title: Isotopic analysis of cosmic rays by the Cerenkov-Cerenkov
slowing-down method
Authors: Meyer, J. P.
1975STIA...7532534M Altcode:
The performance of a large-scale Cerenkov-Cerenkov slowing-down
set-up for isotope analysis in the 1-2 GeV/n region is analysed. Such
a setup should permit isotopic analysis of all nuclei between neon and
nickel with rms mass errors less than 0.5 amu and less than 1 amu over,
respectively, approximately 250 MeV/n and approximately 500 MeV/n energy
ranges. The background associated with the very high rate of nuclear
interactions in the instrument (75 percent) should be eliminated by
a triple redundancy in the charge measurement. These estimates are
based largely on experience gained from Danish-French balloon flights
and from runs at the Berkeley Bevatron.
---------------------------------------------------------
Title: Isotopic Composition of Cosmic Rays
Authors: Meyer, J. P.
1975ICRC...11.3698M Altcode: 1975ICRC...14.3698M
No abstract at ADS
---------------------------------------------------------
Title: Pathlength Distribution and Source Composition of Cosmic
Ray Nuclei
Authors: Meneguzzi, M.; Cesarsky, C. J.; Meyer, J. P.
1975ICRC...12.4183M Altcode: 1975ICRC...14.4183M
No abstract at ADS
---------------------------------------------------------
Title: Galactic Cosmic Ray Particles - State of the Situation and
Prospective
Authors: Meyer, J. P.
1975hea..conf..165M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Cross Sections for Atmospheric Corrections
Authors: Meyer, J. P.; Cassé, M.; Westergaard, N.
1975ICRC...12.4144M Altcode: 1975ICRC...14.4144M
No abstract at ADS
---------------------------------------------------------
Title: Isotopic Analysis of GeV Heavy Nuclei by Differential
Slowing Down.
Authors: Cassé, M.; Goret, P.; Koch, L.; Maubras, Y.; Mestreau, P.;
Meyer, J. P.; Roussel, D.; Soutoul, A.; Valot, P.; Linney, A. D.
1973ICRC....4.2901C Altcode: 1973ICRC...13.2901C
No abstract at ADS
---------------------------------------------------------
Title: Deuterons and He^{3} formation and destruction in proton
induced spallation of light nuclei (Z <= 8)
Authors: Meyer, J. P.
1972A&AS....7..417M Altcode:
With the aim of interpreting the deuteron and He3 abundances in galactic
cosmic radiation, we survey: (i) their production cross sections and
reaction kinematics in p-p, p-He3, p-He4 and p (CNO) interactions, with
special emphasis on the p-He4 reactions, (ii) their destruction cross
sections in p-d and p-He8 reactions, and (iii) the p-p, p-d and p-He4
elastic scattering cross sections. The experimental data are thoroughly
discussed and the "neutron data" reinterpreted in terms of the mirror
proton induced reaction. Whenever reliable observations are lacking,
tentative extrapolations are made, based on (i) expected similarities
with the nucleonnucleon cross sections behaviour, and (ii) the need
for consistancy with the total and the inelastic cross sections. Key
words: Deuteron - Helium 3 - Nuclear Cross sections - Cosmic Rays
---------------------------------------------------------
Title: Cross Sections for the Formation and Destruction of Cosmic
Ray Deuterons and <SUP>3</SUP>He Nuclei. (Abstract)
Authors: Meyer, J. P.
1971ICRC....1..168M Altcode: 1971ICRC...12..168M
No abstract at ADS
---------------------------------------------------------
Title: Cosmic Ray Deuterons and <SUP>3</SUP>He, Interplanetary
Deceleration and Energy Spectra of Sources. (Abstract)
Authors: Meyer, J. -P.
1971ICRC....1..169M Altcode: 1971ICRC...12..169M
No abstract at ADS
---------------------------------------------------------
Title: Interplanetary Deceleration and the Significance of the
Observed Cosmic Ray Deuteron and <SUP>3</SUP>He Fluxes
Authors: Meyer, J. P.
1971icpc.conf..235M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Cross Sections for the Formation and Destruction of Cosmic
Ray Deuterons and <SUP>3</SUP>He Nuclei
Authors: Meyer, J. -P.
1971ICRC....5.1740M Altcode: 1971ICRC...12.1740M
No abstract at ADS
---------------------------------------------------------
Title: Charge composition of relativistic primary cosmic rays between
beryllium and iron.
Authors: Casse, M.; Corydon-Petersen, O.; Dayton, B.; Koch, L.; Lund,
N.; Melgaard, K.; Mestreau, P.; Meyer, J. P.; Omø, K.; Risbo, T.;
Roussel, D.
1971spre.conf.1397C Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Chemical Composition of Heavy Cosmic Ray Nuclei above 5 GV.
Authors: Casse, M.; Koch, L.; Lund, N.; Meyer, J. -P.; Peters, B.;
Soutoul, A.; Tandon, S. N.
1971ICRC....1..241C Altcode: 1971ICRC...12..241C
No abstract at ADS
---------------------------------------------------------
Title: Cosmic Ray Deuterons and He<SUP>3</SUP> Interplanetary
Deceleration and Energy Spectra of Sources
Authors: Meyer, J. -P.
1971ICRC....7.2565M Altcode: 1971ICRC...12.2565M
No abstract at ADS
---------------------------------------------------------
Title: Galactic Cosmic Ray Deuterous and Energy Spectra of Sources
Authors: Meyer, J. -P.
1970ApL.....7...61M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Measurement of the Broadening of Silicon Lines by Electrons
and Hydrogen Atoms
Authors: Meyer, J.; Beck, R. J.
1970A&A.....8...93M Altcode:
The shift and width of two astrophysically important silicon line are
investigated using a pressurized hydrogen plasma jet. The influence
of Stark effect interactions with free electrons and of mi der Waals
interactions with hydrogen atoms on the lines are determined and
the results are compared with theoretical values. The deviations
from theory are discussed separately for the case of Stark effect
interactions and for that of van der Waals interactions.
---------------------------------------------------------
Title: Radiative transition probabilities between the 3p<SUP>5</SUP>4p
and 3p<SUP>5</SUP>4s configurations of neutral argon.
Authors: Nodwell, R. A.; Meyer, J.; Jacobson, T.
1970JQSRT..10..335N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Investigation of pressure broadening of a neon line using
Zeeman scanning technique.
Authors: Meyer, J.; Burnett, J. C.; Stansfield, B.
1970JQSRT..10..799M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Measurement and interpretation of the isotopic composition
of hydrogen and helium cosmic-ray nuclei below 75 MeV/nucleon
Authors: Meyer, J. P.; Hagge, Donald E.; McDonald, Frank B.
1968CaJPS..46..503M Altcode: 1968CaJPh..46S.503M; 1968CaJPh..46..503M; 1968ICRC...10..503M
No abstract at ADS
---------------------------------------------------------
Title: Zur deutung eines scheinbaren mondeinflusses im spektrum der
erdmagnetischen aktivität
Authors: Meyer, J.
1966E&PSL...1..392M Altcode:
It is shown that the secondary maxima near 25.8 and 29.6 days in
the spectrum of geomagnetic activity can fully be understood by
an annual amplitude modulation in the recurrence tendency of M-type
disturbances. This disproves the necessity of assuming lunar influences
on geomagnetic activity, in agreement with the result of Bartels.
---------------------------------------------------------
Title: A note concerning the best observing times during sunspot
minimum
Authors: Meyer, J.
1966E&PSL...1..280M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Use of semiconductor telescopes in charge and energy
spectrometry of cosmic particles
Authors: Engelmann, J.; Koch, I.; Meyer, J. P.
1965ICRC....1..419E Altcode: 1965ICRC....9..419E
No abstract at ADS
---------------------------------------------------------
Title: Object Lowell Observatory
Authors: Esclangon, M. E.; de Grandchamp; Canavaggia; Mineur; Barbier;
Baade, W.; Shapley, H.; Leuschner, A. O.; Bower, E. C.; Whipple,
F. L.; Meyer
1930IAUC..268....1E Altcode:
Observations. In Circulaire No. 8 D (Service des informations rapides)
M. E. Esclangon, Director of the observatory Paris, publishes the
following observations made at Paris observatory (Equatorial of the
Carte du Ciel; observers: de Grandchamp, Canavaggia, Mineur, Barbier;
computers: Mineur, Canavaggia, Barbier): 1930 U.T. R.A. (1930.0)
Decl. March 26 21h32m5 7 15 31.17 +22 8 17.8 27 21 35.0 7 15 31.09 +22
8 24.4 28 21 44.0 7 15 30.63 +22 8 26.4 31 21 7.0 7 15 30.21 +22 8 40.7
April 3 20 7.0 7 15 30.77 +22 8 50.2 Dr. W. Baade at the observatory
Bergedorf sends the following positions: 1930 U.T. R.A. (1930.0)
Decl. March 30 19h47m 4s 7 15 30.23 +22 8 33.6 April 3 23 6 20 7
15 30.84 +22 8 48.8 We have received the following telegram from
Prof. Shapley: "Leuschner telegraphs preliminary investigation Lowell
observatory object by Bower and Whipple results in group of solutions
giving approximate present distance forty one astronomical units
inclination 17 deg. longitude node 109 deg. Observations chiefly
by Meyer Lick Observatory March 16th to April 4th are accurately
represented by orbits varying from near circle to parabola with
perihelion distance 17 astronomical units." An Observation Circular from
the Lowell Observatory of 1930 March 13 gives details about the search
for a transneptunian planet, the discovery of the new object on plates
of 1930 Jan. 21, 23 and 29 and about the observations since that time.
---------------------------------------------------------
Title: Les Obseques de Camille Flammarion.
Authors: Touchet, Em.; Feuillet, A.; Guglielminetti; de Borssat,
Xavier; Bidault de L'Isle, G.; Meyer, Jean; Baillaud, B.; Lallemand,
Ch.; Salzedo, A.; Appell, Paul; Reibel, Charles; Painleve, Paul
1925LAstr..39R.309T Altcode:
No abstract at ADS
