排序方式: 共有49条查询结果,搜索用时 125 毫秒
31.
R. Karrer P. Bochsler C. Giammanco F. M. Ipavich J. A. Paquette P. Wurz 《Space Science Reviews》2007,130(1-4):317-321
Using the Mass Time-of-Flight Spectrometer (MTOF)—part of the Charge, Elements, Isotope Analysis System (CELIAS)—onboard the
Solar Heliospheric Observatory (SOHO) spacecraft, we derive the nickel isotopic composition for the isotopes with mass 58,
60 and 62 in the solar wind. In addition we measure the elemental abundance ratio of nickel to iron. We use data accumulated
during ten years of SOHO operation to get sufficiently high counting statistics and compare periods of different solar wind
velocities. We compare our values with the meteoritic ratios, which are believed to be a reliable reference for the solar
system and also for the solar outer convective zone, since neither element is volatile and no isotopic fractionation is expected
in meteorites. Meteoritic isotopic abundances agree with the terrestrial values and can thus be considered to be a reliable
reference for the solar isotopic composition. The measurements show that the solar wind elemental Ni/Fe-ratio and the isotopic
composition of solar wind nickel are consistent with the meteoritic values. This supports the concept that low-FIP elements
are fed without relative fractionation into the solar wind. Our result also confirms the absence of substantial isotopic fractionation
processes for medium and heavy ions acting in the solar wind. 相似文献
32.
Høg E. Pagel B.E.J. Portinari L. Thejll P.A. Macdonald J. Girardi L. 《Space Science Reviews》1998,84(1-2):115-126
The primordial helium abundance YP is important for cosmology and the ratio Y/Z of the changes relative to primordial abundances constrains models of stellar evolution. While the most accurate estimates of YP come from emission lines in extragalactic H II regions, they involve an extrapolation to zero metallicity which itself is closely tied up with the slope Y/Z. Recently certain systematic effects have come to light in this exercise which make it useful to have an independent estimate of Y/Z from fine structure in the main sequence of nearby stars. We derive such an estimate from Hipparcos data for stars with Z Z and find values between 2 and 3, which are consistent with stellar models, but still have a large uncertainty. 相似文献
33.
The chemical composition of comet nuclei derived from current data on interstellar dust ingredients and comet dust and coma
molecules are shown to be substantially consistent with each other in both refractory and volatile components. When limited
by relative cosmic abundances the water in comet nuclei is constrained to be close to 30% by mass and the refractory to volatile
ratio is close to 1:1. The morphological structure of comet nuclei, as deduced from comet dust infrared continuum and spectral
emission properties, is described by a fluffy (porous) aggregate of tenth micron silicate core-organic refractory mantle particle
on which outer mantles of predominantly H2O ices contain embedded carbonaceous and polycyclic aromatic hydrocarbon (PAH) type particles of size in the of 1 - 10nm range.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
34.
The Local Interstellar Cloud (LIC) surrounds the Solar System and sets the boundary conditions for the heliosphere. Using
both in situ and absorption line data towards ε CMa we are able to constrain both the ionization and the gas phase abundances of the LIC gas at the Solar Location. We find
that the abundances are consistent with all of the carbonaceous dust grains having been destroyed, and in fact with a supersolar
abundance of C. The constituents of silicate grains, Si, Mg, and Fe, appear to be sub-solar, indicating that silicate dust
is present in the LIC. N, O and S are close to the solar values. 相似文献
35.
The differences between the composition of Galactic cosmic rays and that of the interstellar medium are manifold, and they
contain a wealth of information about the varying processes that created them. These differences reveal much about the initial
mixing of freshly synthesized matter, the chemistry and differentiation of the interstellar medium, and the mechanisms and
environment of ion injection and acceleration. Here we briefly explore these processes and show how they combine to create
the peculiar, but potentially universal, composition of the cosmic rays and how measurements of the composition can provide
a unique measure of the mixing ratio of the fresh supernova ejecta and the old interstellar medium in this initial phase of
interstellar mixing.
In particular, we show that the major abundance differences between the cosmic rays and the average interstellar medium can
all result from cosmic ray ion injection by sputtering and scattering from fast refractory oxide grains in a mix of fresh
supernova ejecta and old interstellar material. Since the bulk of the Galactic supernovae occur in the cores of superbubbles,
the bulk of the cosmic rays are accelerated there out of such a mix. We show that the major abundance differences all imply
a mixing ratio of the total masses of fresh supernova ejecta and old interstellar material in such cores is roughly 1 to 4.
That means that the metallicity of ∼3 times solar, since the ejecta has a metallicity of ∼8 times that of the present interstellar
medium. 相似文献
36.
Sylvie Vauclair 《Space Science Reviews》1998,85(1-2):71-78
Element settling inside the Sun now becomes detectable from the comparison of the observed oscillation modes with the results
of the theoretical models. This settling is due, not only to gravitation, but also to thermal diffusion and radiative acceleration
(although this last effect is small compared to the two others). It leads to abundance variations of helium and heavy elements
of ≅ 10% below the convective zone. Although not observable from spectroscopy, such variations lead to non-negligible modifications
of the solar internal structure and evolution. Helioseismology is a powerful tool to detect such effects, and its positive
results represent a great success for the theory of stellar evolution. Meanwhile, evidences are obtained that the element
settling is slightly smoothed down, probably due to mild macroscopic motions below the convective zone. Additional observations
of the abundances of both 7Li and 3He lead to specific constraints on these particular motions.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
37.
Michael Loewenstein David S. Davis 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(12):1972-1974
We discuss the elemental composition in the hot ISM of elliptical galaxies derived from new and recent X-ray spectral analysis in the context of new phenomenological models of their chemical evolution. Star formation histories, the IMF, the astrophysics of supernovae, and the nature of galactic winds impact the metal content and relative abundances in the hot ISM. We evaluate how X-ray spectroscopy may be utilized to deconstruct how elliptical galaxies, and the stellar populations that compose them, form and evolve, with an emphasis on present and future high resolution spectroscopic analysis. 相似文献
38.
A brief review is presented of our current understanding of the evolution of the Milky Way disk and of its relevance to "cosmic chemical evolution" studies. The implications of this understanding for the evolution of deuterium are emphasized. 相似文献
39.
We are making precise determinations of the abundance of the light isotope of helium, 3He. The 3He abundance in Milky Way sources impacts stellar evolution, chemical evolution, and cosmology. The abundance of 3He is derived from measurements of the hyperfine transition of 3He+ which has a rest wavelength of 3.46 cm (8.665 GHz). As with all the light elements, the present interstellar 3He abundance results from a combination of Big Bang Nucleosynthesis (BBNS) and stellar nucleosynthesis. We are measuring the
3He abundance in Milky Way H ii regions and planetary nebulae (PNe). The source sample is currently comprised of 60 H ii regions and 12 PNe. H ii regions are examples of zero-age objects that are young relative to the age of the Galaxy. Therefore their abundances chronicle
the results of billions of years of Galactic chemical evolution. PNe probe material that has been ejected from low-mass (M≤ 2M
⊙) to intermediate-mass (M∼2–5M
⊙) stars to be further processed by future stellar generations. Because the Milky Way ISM is optically thin at centimeter wavelengths,
our source sample probes a larger volume of the Galactic disk than does any other light element tracer of Galactic chemical
evolution. The sources in our sample possess a wide range of physical properties (including object type, size, temperature,
excitation, etc.). The 3He abundances we derive have led to what has been called “The 3He Problem”. 相似文献
40.
N. Werner F. Durret T. Ohashi S. Schindler R. P. C. Wiersma 《Space Science Reviews》2008,134(1-4):337-362
Because of their deep gravitational potential wells, clusters of galaxies retain all the metals produced by the stellar populations
of the member galaxies. Most of these metals reside in the hot plasma which dominates the baryon content of clusters. This
makes them excellent laboratories for the study of the nucleosynthesis and chemical enrichment history of the Universe. Here
we review the history, current possibilities and limitations of the abundance studies, and the present observational status
of X-ray measurements of the chemical composition of the intra-cluster medium. We summarise the latest progress in using the
abundance patterns in clusters to put constraints on theoretical models of supernovae and we show how cluster abundances provide
new insights into the star-formation history of the Universe. 相似文献