136 research outputs found
The place of the Sun among the Sun-like stars
Context. Monitoring of the photometric and chromospheric HK emission data
series of stars similar to the Sun in age and average activity level showed
that there is an empirical correlation between the average stellar
chromospheric activity level and the photometric variability. In general, more
active stars show larger photometric variability. Interestingly, the
measurements and reconstructions of the solar irradiance show that the Sun is
significantly less variable than indicated by the empirical relationship. Aims.
We aim to identify possible reasons for the Sun to be currently outside of this
relationship. Methods. We employed different scenarios of solar HK emission and
irradiance variability and compared them with available time series of Sun-like
stars. Results. We show that the position of the Sun on the diagram of
photometric variability versus chromospheric activity changes with time. The
present solar position is different from its temporal mean position as the
satellite era of continuous solar irradiance measurements has accidentally
coincided with a period of unusually high and stable solar activity. Our
analysis suggests that although present solar variability is significantly
smaller than indicated by the stellar data, the temporal mean solar variability
might be in agreement with the stellar data. We propose that the continuation
of the photometric program and its expansion to a larger stellar sample will
ultimately allow us to constrain the historical solar variability.Comment: 10 pages, 5 figures, accepted for publication in
Astronomy&Astrophysic
Sun-as-a-star Observation of White-Light Flares
Solar flares radiates energy at all wavelengths, but the spectral
distribution of this energy is still poorly known. White-light continuum
emission is sometimes observed and the flares are then termed "white-light
flares" (WLF). In this paper, we investigate if all flares are white-light
flares and how is the radiated energy spectrally distributed. We perform a
superposed epoch analysis of spectral and total irradiance measurements
obtained since 1996 by the SOHO and GOES spacecrafts at various wavelength,
from Soft X-ray to the visible domain. The long-term record of solar irradiance
and excellent duty cycle of the measurements allow us to detect a signal in
visible irradiance even for moderate (C-class) flares, mainly during the
impulsive phase. We identify this signal as continuum emission emitted by
white-light flares, and find that it is consistent with a blackbody emission at
~9000K. We estimate for several sets of flares the contribution of the WL
continuum and find it to be of ~70% of the total radiated energy. We re-analyse
the X17 flare that occurred on 28 October 2003 and find similar results. This
paper brings evidence that all flares are white-light flares and that the
white-light continuum is the main contributor to the total radiated energy;
this continuum is consistent with blackbody spectrum at ~9000K. These
observational results are important in order to understand the physical
mechanisms during flares and open the way to a possible contribution of flares
to TSI variations
The Influence of Solar Flares on the Lower Solar Atmosphere: Evidence from the Na D Absorption Line Measured by GOLF/SOHO
Solar flares presumably have an impact on the deepest layers of the solar
atmosphere and yet the observational evidence for such an impact is scarce.
Using ten years of measurements of the Na D and Na D Fraunhofer
lines, measured by GOLF onboard SOHO, we show that this photospheric line is
indeed affected by flares. The effect of individual flares is hidden by solar
oscillations, but a statistical analysis based on conditional averaging reveals
a clear signature. Although GOLF can only probe one single wavelength at a
time, we show that both wings of the Na line can nevertheless be compared. The
varying line asymmetry can be interpreted as an upward plasma motion from the
lower solar atmosphere during the peak of the flare, followed by a downward
motion.Comment: 13 pages, 7 figure
Chlorine-bearing species and the 37Cl/35Cl isotope ratio in the coma of comet 67P/Churyumov-Gerasimenko
A full-mission analysis of Cl-bearing species in the coma of comet 67P/Churyumov-Gerasimenko has been conducted using data from the Rosetta ROSINA/DFMS mass spectrometer. This contribution will focus on the challenges encountered to relate DFMS data on Cl-bearing species to the neutral abundances at the comet.DFMS was operated in neutral mode, in which electron impact ionizes a fraction of the incoming neutral gas in the ion source. Only ions in a narrow range around a certain commanded mass-over-charge ratio (m/z) pass through the mass analyser at a time and impact on a micro-channel plate (MCP), creating an electron avalanche that is recorded by a Linear Electron Detector Array chip with two rows of 512 pixels each (LEDA A and LEDA B). Data are obtained as Analog-to-Digital Converter (ADC) counts as a function of LEDA pixel number. The instrument scans over a sequence of m/z values.A well-defined approach exists to convert ADC counts as a function of pixel number to the number of ions that were detected on the MCP. However, to relate the number of ions detected this way to the abundance of neutrals in the coma gas, the sensitivity for each neutral needs to be known. The sensitivity for a certain neutral takes into account the total ionization cross section for the neutral and product ion fraction, instrument transmission and secondary electron yield for each product ion. Sensitivities can be determined experimentally by introducing the neutrals in the DFMS instrument copy in the laboratory, but such data are not available for Cl-bearing species and an alternative approach needs to be used. Fortunately, the use of ratios cancels out some of the factors that play a role in the sensitivity. As an example, for the 37Cl/35Cl ratio, total ionization cross sections and product ion fractions can be considered identical. In the case of 37Cl/35Cl, taking into account the sensitivity results in a correction of more than 15%, mainly due to the secondary electron yield.The 37Cl/35Cl ratio does not appear to change appreciably throughout the mission and is compared with known values from other solar system objects. The Cl/HCl ratio obtained with DFMS indicates that there must be at least one additional chlorine-bearing species on the comet next to HCl, CH3Cl and NH4Cl, the identity of which is unknown at this time
Atmospheric Escape Processes and Planetary Atmospheric Evolution
The habitability of the surface of any planet is determined by a complex
evolution of its interior, surface, and atmosphere. The electromagnetic and
particle radiation of stars drive thermal, chemical and physical alteration of
planetary atmospheres, including escape. Many known extrasolar planets
experience vastly different stellar environments than those in our Solar
system: it is crucial to understand the broad range of processes that lead to
atmospheric escape and evolution under a wide range of conditions if we are to
assess the habitability of worlds around other stars. One problem encountered
between the planetary and the astrophysics communities is a lack of common
language for describing escape processes. Each community has customary
approximations that may be questioned by the other, such as the hypothesis of
H-dominated thermosphere for astrophysicists, or the Sun-like nature of the
stars for planetary scientists. Since exoplanets are becoming one of the main
targets for the detection of life, a common set of definitions and hypotheses
are required. We review the different escape mechanisms proposed for the
evolution of planetary and exoplanetary atmospheres. We propose a common
definition for the different escape mechanisms, and we show the important
parameters to take into account when evaluating the escape at a planet in time.
We show that the paradigm of the magnetic field as an atmospheric shield should
be changed and that recent work on the history of Xenon in Earth's atmosphere
gives an elegant explanation to its enrichment in heavier isotopes: the
so-called Xenon paradox
The Main Belt Comets and ice in the Solar System
We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies
Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko
Several sulphur-bearing species have already been observed in different families of comets. However, the knowledge on the minor sulphur species is still limited. The comet’s sulphur inventory is closely linked to the pre-solar cloud and holds important clues to the degree of reprocessing of the material in the solar nebula and during comet accretion. Sulphur in pre-solar clouds is highly depleted, which is quite puzzling as the S/O ratio in the diffuse interstellar medium is cosmic. This work focuses on the abundance of the previously known species H2S, OCS, SO, S2, SO2 and CS2 in the coma of comet 67P/Churyumov–Gerasimenko measured by Rosetta Orbiter Spectrometer for Ion and Neutral Analysis/Double Focusing Mass Spectrometer between equinox and perihelion 2015. Furthermore, we present the first detection of S3, S4, CH3SH and C2H6S in a comet, and we determine the elemental abundance of S/O in the bulk ice of (1.47 ± 0.05) × 10−2. We show that SO is present in the coma originating from the nucleus, but not CS in the case of 67P, and for the first time establish that S2 is present in a volatile and a refractory phase. The derived total elemental sulphur abundance of 67P is in agreement with solar photospheric elemental abundances and shows no sulphur depletion as reported for dense interstellar clouds. Also the presence of S2 at heliocentric distances larger than 3 au indicates that sulphur-bearing species have been processed by radiolysis in the
pre-solar cloud and that at least some of the ice from this cloud has survived in comets up the present
Halogens as tracers of protosolar nebula material in comet 67P/Churyumov–Gerasimenko
We report the first in situ detection of halogens in a cometary coma, that of 67P/ChuryumovGerasimenko. Neutral gas mass spectra collected by the European Space Agency’s Rosetta spacecraft during four periods of interest from the first comet encounter up to perihelion indicate that the main halogen-bearing compounds are HF, HCl and HBr. The bulk elemental abundances relative to oxygen are ~8.9 × 10⁻⁵ for F/O, ~1.2 × 10⁻⁴ for Cl/O and ~2.5 × 10⁻⁶ for Br/O, for the volatile fraction of the comet. The cometary isotopic ratios for ³⁷Cl/³⁵Cl and ⁸¹Br/⁷⁹Br match the Solar system values within the error margins. The observations point to an origin of the hydrogen halides in molecular cloud chemistry, with frozen hydrogen halides on dust grains, and a subsequent incorporation into comets as the cloud condensed and the Solar system formed
Evidence for distributed gas sources of hydrogen halides in the coma of comet 67P/Churyumov–Gerasimenko
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