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1.
Information about the composition of volatiles in the Martian atmosphere and interior derives from Viking spacecraft and ground-based measurements, and especially from measurements of volatiles trapped in Martian meteorites, which contain several distinct components. One volatile component, found in impact glass in some shergottites, gives the most precise measurement to date of the composition of Martian atmospheric Ar, Kr, and Xe, and also contains significant amounts of atmospheric nitrogen showing elevated 15N/14N. Compared to Viking analyses, the 36Ar/132Xe and 84Kr/132Xe elemental ratios are larger in shergottites, the 129Xe/132Xe ratio is similar, and the 40Ar/36Ar and 36Ar/38Ar ratios are smaller. The isotopic composition of atmospheric Kr is very similar to solar Kr, whereas the isotopes of atmospheric Xe have been strongly mass fractionated in favor of heavier isotopes. The nakhlites and ALH84001 contain an atmospheric component elementally fractionated relative to the recent atmospheric component observed in shergottites. Several Martian meteorites also contain one or more Martian interior components that do not show the mass fractionation observed in atmospheric noble gases and nitrogen. The D/H ratio in the atmosphere is strongly mass fractionated, but meteorites contain a distinct Martian interior hydrogen component. The isotopic composition of Martian atmospheric carbon and oxygen have not been precisely measured, but these elements in meteorites appear to show much less variation in isotopic composition, presumably in part because of buffering of the atmospheric component by larger condensed reservoirs. However, differences in the oxygen isotopic composition between meteorite silicate minerals (on the one hand) and water and carbonates indicate a lack of recycling of these volatiles through the interior. Many models have been presented to explain the observed isotopic fractionation in Martian atmospheric N, H, and noble gases in terms of partial loss of the planetary atmosphere, either very early in Martian history, or over extended geological time. The number of variables in these models is large, and we cannot be certain of their detailed applicability. Evolutionary data based on the radiogenic isotopes (i.e., 40Ar/36Ar, 129Xe/132Xe, and 136Xe/132Xe ratios) are potentially important, but meteorite data do not yet permit their use in detailed chronologies. The sources of Mars' original volatiles are not well defined. Some Martian components require a solar-like isotopic composition, whereas volatiles other than the noble gases (C, N, and H2O) may have been largely contributed by a carbonaceous (or cometary) veneer late in planet formation. Also, carbonaceous material may have been the source of moderate amounts of water early in Martian history. 相似文献
2.
Yann Alibert Christoph Mordasini Olivier Mousis Willy Benz 《Space Science Reviews》2005,116(1-2):77-95
We present models of giant planet formation, taking into account migration and disk viscous evolution. We show that migration
can significantly reduce the formation timescale bringing it in good agreement with typical observed disk lifetimes. We then
present a model that produces a planet whose current location, core mass and total mass are comparable with the one of Jupiter.
For this model, we calculate the enrichments in volatiles and compare them with the one measured by the Galileo probe. We
show that our models can reproduce both the measured atmosphere enrichments and the constraints derived by Guillot et al. (2004), if we assume the accretion of planetesimals with ices/rocks ratio equal to 4, and that a substantial amount of CO2 was present in vapor phase in the solar nebula, in agreement with ISM measurements. 相似文献
3.
The measured D/H ratios in interstellar environments and in the solar system are reviewed. The two extreme D/H ratios in solar
system water - (720±120)×10−6 in clay minerals and (88±11)×10−6 in chondrules, both from LL3 chondritic meteorites - are interpreted as the result of a progressive isotopic exchange in
the solar nebula between deuterium-rich interstellar water and protosolar H2. According to a turbulent model describing the evolution of the nebula (Drouart et al., 1999), water in the solar system cannot be a product of thermal (neutral) reactions occurring in the solar nebula. Taking
720×10−6 as a face value for the isotopic composition of the interstellar water that predates the formation of the solar nebula, numerical
simulations show that the water D/H ratio decreases via an isotopic exchange with H2. During the course of this process, a D/H gradient was established in the nebula. This gradient was smoothed with time and
the isotopic homogenization of the solar nebula was completed in 106 years, reaching a D/H ratio of 88×10−6. In this model, cometary water should have also suffered a partial isotopic re-equilibration with H2. The isotopic heterogeneity observed in chondrites result from the turbulent mixing of grains, condensed at different epochs
and locations in the solar nebula. Recent isotopic determinations of water ice in cold interstellar clouds are in agreement
with these chondritic data and their interpretation (Texeira et al., 1999).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
4.
Two fractionation models are applied to the problem of generating the widely distributed “Q-component” noble gases in meteorites
from the solar-like isotopic and elemental compositions that presumably characterized the early solar accretion disk. Noble
gas fractionation by mass-dependent dissipation of the solar nebula, as suggested by Ozima et al. (1998), is examined in the context of a model developed by Johnstone et al. (1998) for accretion disk photoevaporation driven by intense UV radiation from a neighboring giant star. Hydrodynamic escape
of heavier species entrained in hydrogen outflow from the UV-heated outer regions of the disk can generate substantial noble
gas fractionations, but they do not match the observed Q-component isotopic pattern and moreover require the physically unrealistic
assumption that the fractionated gases are confined to the heated disk boundary zone, without mixing with the interior nebula,
for long periods of time. It seems more likely that hydrodynamic outflow is actually established below this zone, in the body
of the disk. In this case fractionations are governed by Rayleigh distillation of the entire remaining nebula, and are negligible
at the time when disk erosion is halted by the gravitational potential of the young sun embedded in the disk.
A “local” model of noble gas fractionation by hydrodynamic blowoff of transient, methane-rich atmospheres outgassed from the
interiors of large primitive planetesimals (Pepin, 1991) is updated and assessed against current data. Degassed atmospheres
are assumed to contain isotopically solar noble gases except for an additional nucleogenic Xe component that contributes primarily
to the two heaviest isotopes; there is evidence that this same component is present at varying levels in other solar-system
volatile reservoirs, possibly reflecting a compositional change with time in the solar nebula. Single fixed values for the
two free parameters in the blowoff modeling equations can generate fractionated Xe, Kr, Ar and Ne compositions in the residual
atmosphere that closely match observed meteoritic isotopic distributions, and Q-gas elemental ratios are approximated by adsorption
of fractionated gases on planetesimal surface grains using plausible values of relative Henry Law constants. Additional requirements
for adsorption of sufficient absolute amounts of Q-gases on carrier grains, and their subsequent ejection to space, mixing
in the nebula, and dispersal into meteorite bodies, are examined in the context of current models for body sizes and dynamical
evolution in an early mass-rich asteroid belt (Chambers and Wetherill, 2001). Despite its ability to replicate isotopic compositions,
uncertainties about the environments in which the blowoff model can successfully operate suggest that there is, as yet, no
entirely satisfactory understanding of how the Q-component noble gases might have evolved from solar-like precursor compositions.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
5.
The gas flux from a volatile icy-dust mixture is computed using a comet nucleus thermal model in order to study the evolution
of CO outgassing during several apparitions from long-period Comet Hale-Bopp and short-period Comet Wirtanen. The comet model
assumes a spherical, porous body containing a dust component, one major ice component (H2O), and one minor ice component of higher volatility (CO). The initial chemical composition is assumed to be homogeneous.
The following processes are taken into account: heat and gas diffusion inside the rotating nucleus; release of outward diffusing
gas from the comet nucleus; chemical differentiation by sublimation of volatile ices in the surface layers and recondensation
of gas in deeper, cooler layers. A 2-D time dependent solution is obtained through the dependence of the boundary conditions
on the local solar illumination as the nucleus rotates. The model for Comet Hale-Bopp was compared with observational measurements
(Biver et al., 1999). The best agreement was obtained for a model with amorphous water ice and CO, assuming that a part of the latter is
trapped by the water ice, another part is condensed as an independent ice phase. The model confirms that sublimation of CO
ice at large heliocentric distance produces a gradual increase in the comet's activity as it approaches the Sun. Crystallization
of amorphous water ice begins at 7 AU from the Sun, but no outbursts were found. Seasonal effects and thermal inertia of the
nucleus material lead to larger CO outgassing rates as the comet recedes from the Sun. In the second part of this work the
model was run with the orbital parameters of Comet Wirtanen. Unlike Comet Hale-Bopp, the predicted CO outgassing from Comet
Wirtanen is almost constant throughout its orbit. Such behavior can be explained by a thermally evolved and chemically differentiated
comet nucleus.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
6.
The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the
early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models”
in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A
simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal
formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth.
We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not
much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely
used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation
from the molecular cloud onto the disk, disk evolution and migration of solids.
Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant
amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass
at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment
in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review
likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and
their global composition.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
7.
Pekka Janhunen Annika Olsson Christopher T. Russell Harri Laakso 《Space Science Reviews》2006,122(1-4):89-95
Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms
are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science
299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of
4–5 R
E
(Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance
level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed
conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is
responsible for the energy transfer. 相似文献
8.
W. B. Durham O. Prieto-Ballesteros D. L. Goldsby J. S. Kargel 《Space Science Reviews》2010,153(1-4):273-298
Laboratory measurements of physical properties of planetary ices generate information for dynamical models of tectonically active icy bodies in the outer solar system. We review the methods for measuring both flow properties and thermal properties of icy planetary materials in the laboratory, and describe physical theories that are essential for intelligent extrapolation of data from laboratory to planetary conditions. This review is structured with a separate and independent section for each of the two sets of physical properties, rheological and thermal. The rheological behaviors of planetary ices are as diverse as the icy moons themselves. High-pressure water ice phases show respective viscosities that vary over four orders of magnitude. Ices of CO2, NH3, as well as clathrate hydrates of CH4 and other gases vary in viscosity by nearly ten orders of magnitude. Heat capacity and thermal conductivity of detected/inferred compositions in outer solar system bodies have been revised. Some low-temperature phases of minerals and condensates have a deviant thermal behavior related to paramount water ice. Hydrated salts have low values of thermal conductivity and an inverse dependence of conductivity on temperature, similar to clathrate hydrates or glassy solids. This striking behavior may suit the dynamics of icy satellites. 相似文献
9.
R. Wieler 《Space Science Reviews》1998,85(1-2):303-314
Lunar soil and certain meteorites contain noble gases trapped from the solar wind at various times in the past. The progress
in the last decade to decipher these precious archives of solar history is reviewed. The samples appear to contain two solar
noble gas components with different isotopic composition. The solar wind component resides very close to grain surfaces and
its isotopic composition is identical to that of present-day solar wind. Experimental evidence seems by now overwhelming that
somewhat deeper inside the grains there exists a second, isotopically heavier component. To explain the origin of this component
remains a challenge, because it is much too abundant to be readily reconciled with the known present day flux of solar particles
with energies above those of the solar wind. The isotopic composition of solar wind noble gases may have changed slightly
over the past few Ga, but such a change is not firmly established. The upper limit of ~5% per Ga for a secular increase of
the 3He/4He ratio sets stringent limits on the amount of He that may have been brought from the solar interior to the surface
(cf. Bochsler, 1992). Relative abundances of He, Ne, and Ar in present-day solar wind are the same as the long term average
recorded in metallic Fe grains in meteorites within error limits of some 15-20%. Xe, and to a lesser extent Kr, are enriched
in the solar wind similar to elements with a first ionisation potential < 10 eV, although Kr and Xe have higher FIPs. This
can be explained if the ionisation time governs the FIP effect (Geiss and Bochsler, 1986).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
10.
R. C. Wiens D. S. Burnett C. M. Hohenberg A. Meshik V. Heber A. Grimberg R. Wieler D. B. Reisenfeld 《Space Science Reviews》2007,130(1-4):161-171
The Genesis mission returned samples of solar wind to Earth in September 2004 for ground-based analyses of solar-wind composition,
particularly for isotope ratios. Substrates, consisting mostly of high-purity semiconductor materials, were exposed to the
solar wind at L1 from December 2001 to April 2004. In addition to a bulk sample of the solar wind, separate samples of coronal
hole (CH), interstream (IS), and coronal mass ejection material were obtained. Although many substrates were broken upon landing
due to the failure to deploy the parachute, a number of results have been obtained, and most of the primary science objectives
will likely be met. These objectives include He, Ne, Ar, Kr, and Xe isotope ratios in the bulk solar wind and in different
solar-wind regimes, and 15N/14N and 18O/17O/16O to high precision. The greatest successes to date have been with the noble gases. Light noble gases from bulk solar wind
and separate solar-wind regime samples have now been analyzed. Helium results show clear evidence of isotopic fractionation
between CH and IS samples, consistent with simplistic Coulomb drag theory predictions of fractionation between the photosphere
and different solar-wind regimes, though fractionation by wave heating is also a possible explanation. Neon results from closed
system stepped etching of bulk metallic glass have revealed the nature of isotopic fractionation as a function of depth, which
in lunar samples have for years deceptively suggested the presence of an additional, energetic component in solar wind trapped
in lunar grains and meteorites. Isotope ratios of the heavy noble gases, nitrogen, and oxygen are in the process of being
measured. 相似文献
11.
F.B. McDonald Z. Fujii P. Ferrando B. Heber A. Raviart H. Kunow N. Lal R. Mller-Mellin G. Wibberenz R. McGuire C. Paizis 《Space Science Reviews》2001,97(1-4):321-325
The combination of Voyager 1 (77.9 AU, 34.4° N) and Voyager 2 (61.2 AU, 24.5° S) at moderate heliolatitudes in the distant heliosphere and Ulysses with its unique latitudinal surveys in the inner heliosphere along with IMP 8 and other satellites at 1 AU constitutes a
network of observatories that are ideally suited to study cosmic rays over the solar minimum of cycle 22 and the onset of
solar activity and the long term cosmic ray modulation of cycle 23. Through 2000.7 there have been three well-defined step
decreases in the cosmic ray intensity at 1 AU with the cumulative effect being in good agreement with the net decrease in
cycle 21 at a comparable time in the solar cycle. Over this period the intensity changes at Ulysses are similar to those at 1 AU. In the distant heliosphere the initial decreases appear to be smaller than those at 1 AU. However
the full effects of the interplanetary disturbances producing the most recent and largest step decrease in the inner heliosphere
have not yet reached V-2.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
12.
Paul R. Weissman 《Space Science Reviews》1985,41(3-4):299-349
The modern theory of cometary dynamics is based on Oort's hypothesis that the solar system is surrounded by a spherically symmetric cloud of 1011 to 1012 comets extending out to interstellar distances. Dynamical modeling and analysis of cometary motion have confirmed the ability of the Oort hypothesis to explain the observed distribution of energies for the long-period comet orbits. The motion of comets in the Oort cloud is controlled by perturbations from random passing stars, interstellar clouds, and the galactic gravitational field. Additionally, comets which enter the planetary region are perturbed by the major planets and by nongravitational forces resulting from jetting of volatiles on the surfaces of the cometary nuclei. The current Oort cloud is estimated to have a radius of 6 to 8 × 104 AU, and to contain some 2 × 1012 comets with a total mass of 7 to 8 Earth masses. Evidence has begun to accumulate for the existence of a massive inner Oort cloud extending from just beyond the orbit of Neptune to 104 AU or more, with a population up to 100 times that of the outer Oort cloud. This inner cloud may serve as a reservoir to replenish the outer cloud as comets are stripped away by the various perturbers, and may also provide a more efficient source for the short-period comets. Recent suggestions of an unseen solar companion star or a tenth planet orbiting in the inner cloud and causing periodic comet showers on the Earth are likely unfounded. The formation site of the comets in the Oort cloud was likely the extended nebula accretion disc reaching from about 15 to 500 AU from the forming protosun. Comets which escape from the Oort cloud contribute to the flux of interstellar comets, though capture of interstellar comets by the solar system is extremely unlikely. The existence of Oort clouds around other main sequence stars has been suggested by the detection by the IRAS spacecraft of cool dust shells around about 10% of nearby stars. 相似文献
13.
The intense solar activity centered in March and June 1991 produced some of the largest interplanetary disturbances over the past several solar cycles. For these events the Ulysses EPAC energetic particle observations near 3 AU are compared with those of the Voyager 2 CRS experiment near 35 AU. At Voyager 2 there is a single long-lived event extending over a period of some 6 months while the Ulysses data shows the imprint of individual events as well as the formative stages of the longer lived structure. The average intensity gradient is –17% AU between the 2 spacecraft. At both locations the energy spectra can be represented by an exponential in momentum. The characteristic momentum for protons, (Po)H is on the average 4–5 times larger at 35 AU than at 3 AU and there is a significant change in the (Po)He/(Po)H ratio. However the average H to He ratio is in the range 20–25 for both sets of measurements. 相似文献
14.
It is well established that the prolonged and thorough mixing of numerous nucleosynthetic components that constitutes the
matter in the solar nebula resulted in an essential isotopic homogeneity of the solar system material. This may or may not
be true for the short-lived radionuclides which were injected into or formed within the solar nebula just prior to or during
solar system formation. Distinguishing between their heterogeneous or homogeneous distribution is important because the short-
lived radionuclides are now widely used for the relative chronology of various objects and processes in the early solar system
and as constraints for models of nucleosynthesis. The recent studies of the 53Mn-53Cr isotope system (half life of 53Mn is 3.7 Ma) in various solar system objects have shown that the relative abundance of radiogenic 53Cr is consistent with essentially homogeneous distribution of 53Mn in the asteroid belt. Thus, the relative 53Mn-53Cr chronometer can be directly used for dating samples which originated in the asteroid belt. Importantly, however, all meteorite
groups studied so far indicate a clear excess of 53Cr as compared to Earth and to a lunar sample, which exhibits also a terrestrial 53Cr/52Cr ratio. The results from the Martian (SNC) meteorites show that their 53Cr excesses are less than half of those found in the asteroid belt bodies. Thus, the characteristic 53Cr/52Cr ratio of Mars is intermediate between that of the Earth-Moon system and those of the other meteorites. If these 53Cr variations are viewed as a function of the heliocentric distance, the radial dependence of the relative abundances of radiogenic
53Cr is indicated. This observed gradient can be explained by either an early, volatility controlled, Mn/Cr fractionation within
the nebula or by an initial radial heterogeneous distribution of 53Mn. Although model calculations of the Mn/Cr ratios in the bulk terrestrial planets seem to be inconsistent with the volatility
driven scenario, the precision of these calculations is inadequate for eliminating this possibility. In contrast, recent studies
of the 53Mn-53Cr system in the enstatite chondrites indicate that, while their bulk Mn/Cr ratios are essentially the same as in ordinary
chondrites, the 53Cr excess in bulk enstatite chondrites is three times lower than that in the bulk ordinary chondrites. This difference cannot
be explained by a Mn/Cr fractionation and, thus, strongly suggests that a radial heterogeneous distribution of 53Mn must have existed in at least the early inner solar system. Using the observed gradient and the 53Cr/52Cr ratio of the bulk enstatite chondrites, their parent body(ies) formed at ∼1.4 AU or somewhat closer to the Sun.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
15.
Bruce Fegley Jr. 《Space Science Reviews》2000,92(1-2):177-200
Thermochemical equilibrium calculations predict gas phase, gas-grain, and solid phase reactions as a function of pressure
and temperature in the solar nebula. However, chemical reactions proceed at different rates, which generally decrease exponentially
with decreasing temperature. At sufficiently low temperatures (which vary depending on the specific reaction) there may not
have been enough time for the predicted equilibrium chemistry to have taken place before the local environment cooled significantly
or before the gaseous solar nebula was dispersed. As a consequence, some of the high temperature chemistry established in
sufficiently hot regions of the solar nebula may be quenched or frozen in without the production of predicted low temperature
phases. Experimental studies and theoretical models of three exemplary low temperature reactions, the formation of troilite
(FeS), magnetite (Fe3O4), and hydrous silicates, have been done to quantify these ideas. A comparison of the chemical reaction rates with the estimated
nebular lifetime of 0.1-10 million years indicates that troilite formation proceeded to completion in the solar nebula. Magnetite
formation was much slower and only thin magnetite rims could have formed on metal grains. Hydrous silicate formation is predicted
to be even slower, and hydrous silicates in meteorites and interplanetary dust particles probably formed later on the parent
bodies of these objects, instead of in the solar nebula.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
16.
Solar Nebula Magnetohydrodynamics 总被引:1,自引:0,他引:1
The dynamical state of the solar nebula depends critically upon whether or not the gas is magnetically coupled. The presence
of a subthermal field will cause laminar flow to break down into turbulence. Magnetic coupling, in turn, depends upon the
ionization fraction of the gas. The inner most region of the nebula (≲0.1 AU) is magnetically well-coupled, as is the outermost
region (≳10 AU). The magnetic status of intermediate scales (∼1 AU) is less certain. It is plausible that there is a zone
adjacent to the inner disk in which turbulent heating self-consistently maintains the requisite ionization levels. But the
region adjacent to the active outer disk is likely to be magnetically ``dead.' Hall currents play a significant role in nebular
magnetohydrodynamics.
Though still occasionally argued in the literature, there is simply no evidence to support the once standard claim that differential
rotation in a Keplerian disk is prone to break down into shear turbulence by nonlinear instabilities. There is abundant evidence—numerical,
experimental, and analytic—in support of the stabilizing role of Coriolis forces. Hydrodynamical turbulence is almost certainly
not a source of enhanced turbulence in the solar nebula, or in any other astrophysical accretion disk.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
17.
A major goal of comet research is to determine conditions in the outer solar nebula based on the chemical composition and
structure of comet nuclei. The old view was to use coma abundances directly for the chemical composition of the nucleus. However,
since the composition of the coma changes with heliocentric distance, r, the new view is that the nucleus composition msut be determined from analysis of coma mixing ratios as a function of r. Taking advantage of new observing technology and the early detection of the very active Comet Hale-Bopp (C/1995 O1) allows
us to determine the coma mixing ratios over a large range of heliocentric distances.
In our analysis we assume three sources for the coma gas: (1) the surface of the nucleus (releasing water vapor), (2) the
interior of the porous nucleus (releasing many species more volatile than water), and (3) the distributed source (releasing
gases from ices and hydrocarbon polycondensates trapped and contained in coma dust). Molecules diffusing inside the nucleus
are sublimated by heat transported into the interior. The mixing ratios in the coma are modeled assuming various chemical
compositions and structural parameters of the spinning nucleus as it moves in its orbit from large heliocentric distance through
perihelion.
We have combined several sets of observational data of Comet Hale-Bopp for H2O (from OH) and CO, covering the spectrum range from radio to UV. Many inconsistencies in the data were uncovered and reported
to the observers for a reanalysis. Since post-perihelion data are still sparse, we have combined pre- and post-perihelion
data. The resulting mixing ratio of CO relative to H2O as a function of r is presented with a preliminary analysis that still needs to be expanded further. Our fit to the data indicates that the
total CO release rate (from the nucleus and distributed sources) relative to that of H2O is 30% near perihelion.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
18.
Type III solar radio bursts have been observed from 10 MHz to 10 kHz by satellite experiments above the terrestrial plasmasphere. Solar radio emission in this frequency range results from excitation of the interplanetary plasma by energetic particles propagating outward along open field lines over distances from 5 R
to at least 1 AU from the Sun. This review summarizes the morphology, characteristics and analysis of individual as well as storms of bursts. Substantial evidence is available to show that the radio emission is observed at the second harmonic instead of the fundamental of the plasma frequency. This brings the density scale derived by radio observations into better agreement with direct solar wind density measurements at 1 AU and relaxes the requirement for type III propagation along large density-enhanced regions. This density scale with the measured direction of arrival of the radio burst allows the trajectory of the exciter path to be determined from 10 R
to 1 AU. Thus, for example, the dynamics and gross structure of the interplanetary magnetic field can be investigated by this method. Burst rise times are interpreted in terms of exciter length and dispersion while decay times refer to the radiation damping process. The combination of radio observations at the lower frequencies and in-situ measurements on non-relativistic electrons at 1 AU provide data on the energy range and efficiency of the wave-particle interactions responsible for the radio emission. 相似文献
19.
Microstreams and pressure balance structures in fast solar wind were more easily detected at Ulysses at 2.2 AU over the poles than at Helios at 0.3 AU. This is because solar rotation leads to dynamic interactions between different speed regimes at a rate that depends
on latitude for the same size features. Dynamic interactions make structures more difficult to detect with increasing distance
from the Sun. At solar maximum, Ulysses will sample high latitude solar wind coming from streamers, providing information on fine structure at the tops of streamers
and on the source of slow solar wind. Examples are given here of the detectability of various sized structures at Ulysses when it is over the polar regions of the Sun.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
20.
For nearly fifteen years the Voyager 1 and 2 spacecraft have been detecting an unusual radio emission in the outer heliosphere in the frequency range from about 2 to 3 kHz, Two major events have been observed, the first in 1983–84 and the second in 1992–93. In both cases the onset of the radio emission occurred about 400 days after a period of intense solar activity, the first in mid-July 1982, and the second in May–June 1991. These two periods of solar activity produced the two deepest cosmic ray Forbush decreases ever observed. Forbush decreases are indicative of a system of strong shocks and associated disturbances propagating outward through the heliosphere. The radio emission is believed to have been produced when this system of shocks and disturbances interacted with one of the outer boundaries of the heliosphere, most likely in the vicinity of the the heliopause. The emission is believed to be generated by the shock-driven Langmuir-wave mode conversion mechanism, which produces radiation at the plasma frequency (f
p
) and at twice the plasma frequency (2f
p
). From the 400-day travel time and the known speed of the shocks, the distance to the interaction region can be computed, and is estimated to be in the range from about 110 to 160 AU.Abbreviations PWS
Plasma Wave Subsystem
- AU
Astronomical Unit
- DSN
Deep Space Network
- NASA
National Aeronautics and Space Administration
- GMIR
Global Merged Interaction Region
- MHD
Magnetohydrodynamic
- CME
coronal mass ejection
-
f
p
plasma frequency
- R
radial distance
- AGC
automatic gain control 相似文献