81 research outputs found
UV photodesorption of methanol in pure and CO-rich ices: desorption rates of the intact molecule and of the photofragments
Wavelength dependent photodesorption rates have been determined using
synchrotron radiation, for condensed pure and mixed methanol ice in the 7 -- 14
eV range. The VUV photodesorption of intact methanol molecules from pure
methanol ices is found to be of the order of 10 molecules/photon, that
is two orders of magnitude below what is generally used in astrochemical
models. This rate gets even lower ( 10 molecules/photon) when the
methanol is mixed with CO molecules in the ices. This is consistent with a
picture in which photodissociation and recombination processes are at the
origin of intact methanol desorption from pure CHOH ices. Such low rates
are explained by the fact that the overall photodesorption process is dominated
by the desorption of the photofragments CO, CH, OH, HCO and
CHO/CHOH, whose photodesorption rates are given in this study. Our
results suggest that the role of the photodesorption as a mechanism to explain
the observed gas phase abundances of methanol in cold media is probably
overestimated. Nevertheless, the photodesorption of radicals from methanol-rich
ices may stand at the origin of the gas phase presence of radicals such as
CHO, therefore opening new gas phase chemical routes for the formation of
complex molecules.Comment: 13 pages, 2 figures, 1 tabl
Indirect ultraviolet photodesorption from CO:N2 binary ices - an efficient grain-gas process
UV ice photodesorption is an important non-thermal desorption pathway in many
interstellar environments that has been invoked to explain observations of cold
molecules in disks, clouds and cloud cores. Systematic laboratory studies of
the photodesorption rates, between 7 and 14 eV, from CO:N2 binary ices, have
been performed at the DESIRS vacuum UV beamline of the synchrotron facility
SOLEIL. The photodesorption spectral analysis demonstrates that the
photodesorption process is indirect, i.e. the desorption is induced by a photon
absorption in sub-surface molecular layers, while only surface molecules are
actually desorbing. The photodesorption spectra of CO and N2 in binary ices
therefore depend on the absorption spectra of the dominant species in the
subsurface ice layer, which implies that the photodesorption efficiency and
energy dependence are dramatically different for mixed and layered ices
compared to pure ices. In particular, a thin (1-2 ML) N2 ice layer on top of CO
will effectively quench CO photodesorption, while enhancing N2 photodesorption
by a factors of a few (compared to the pure ices) when the ice is exposed to a
typical dark cloud UV field, which may help to explain the different
distributions of CO and N2H+ in molecular cloud cores. This indirect
photodesorption mechanism may also explain observations of small amounts of
complex organics in cold interstellar environments.Comment: 21 pages 5 figure
X-ray photodesorption of complex organic molecules in protoplanetary disks -- I. Acetonitrile CH3CN
X-rays emitted from pre-main-sequence stars at the center of protoplanetary
disks can induce nonthermal desorption from interstellar ices populating the
cold regions. This X-ray photodesorption needs to be quantified for complex
organic molecules (COMs), including acetonitrile CH3CN, which has been detected
in several disks. We experimentally estimate the X-ray photodesorption yields
of neutral species from pure CH3CN ices and from interstellar ice analogs for
which CH3CN is mixed either in a CO- or H2O-dominated ice. The ices were
irradiated at 15 K by soft X-rays (400-600 eV) from synchrotron light (SOLEIL
synchrotron). X-ray photodesorption was probed in the gas phase via quadrupole
mass spectrometry. X-ray photodesorption yields were derived from the mass
signals and were extrapolated to higher X-ray energies for astrochemical
models. X-ray photodesorption of the intact CH3CN is detected from pure CH3CN
ices and from mixed 13CO:CH3CN ices, with a yield of about 5x10^(-4)
molecules/photon at 560 eV. When mixed in H2O-dominated ices, X-ray
photodesorption of the intact CH3CN at 560 eV is below its detection limit,
which is 10^(-4) molecules/photon. Yields associated with the desorption of
HCN, CH4 , and CH3 are also provided. The derived astrophysical yields
significantly depend on the local conditions expected in protoplanetary disks.
They vary from 10^(-4) to 10(-6) molecules/photon for the X-ray photodesorption
of intact CH3CN from CO-dominated ices. Only upper limits varying from
5x10^(-5) to 5x10^(-7) molecules/photon could be derived for the X-ray
photodesorption of intact CH3CN from H2O-dominated ices. X-ray photodesorption
of intact CH3CN from interstellar ices might in part explain the abundances of
CH3CN observed in protoplanetary disks. The desorption efficiency is expected
to vary with the local physical conditions, hence with the disk region
Wavelength-Dependent UV Photodesorption of Pure and Ices
Context: Ultraviolet photodesorption of molecules from icy interstellar grains can explain observations of cold gas in regions where thermal desorption is negligible. This non-thermal desorption mechanism should be especially important where UV fluxes are high. Aims: and are expected to play key roles in astrochemical reaction networks, both in the solid state and in the gas phase. Measurements of the wavelength-dependent photodesorption rates of these two infrared-inactive molecules provide astronomical and physical-chemical insights into the conditions required for their photodesorption.
Methods: Tunable radiation from the DESIRS beamline at the SOLEIL synchrotron in the astrophysically relevant 7 to 13.6 eV range is used to irradiate pure and thin ice films. Photodesorption of molecules is monitored through quadrupole mass spectrometry. Absolute rates are calculated by using the well-calibrated CO photodesorption rates. Strategic and isotopolog mixtures are used to investigate the importance of dissociation upon irradiation. Results: photodesorption mainly occurs through excitation of the state and subsequent desorption of surface molecules. The observed vibronic structure in the photodesorption spectrum, together with the absence of formation, supports that the photodesorption mechanism of is similar to CO, i.e., an indirect DIET (Desorption Induced by Electronic Transition) process without dissociation of the desorbing molecule. In contrast, photodesorption in the 7â13.6 eV range occurs through dissociation and presents no vibrational structure. Conclusions: Photodesorption rates of and integrated over the far-UV field from various star-forming environments are lower than for CO. Rates vary between and photodesorbed molecules per incoming photon.Astronom
Spectrally-resolved UV photodesorption of CH4 in pure and layered ices
Context. Methane is among the main components of the ice mantles of
insterstellar dust grains, where it is at the start of a rich solid-phase
chemical network. Quantification of the photon-induced desorption yield of
these frozen molecules and understanding of the underlying processes is
necessary to accurately model the observations and the chemical evolution of
various regions of the interstellar medium. Aims. This study aims at
experimentally determining absolute photodesorption yields for the CH4 molecule
as a function of photon energy. The influence of the ice composition is also
investigated. By studying the methane desorption from layered CH4:CO ice,
indirect desorption processes triggered by the excitation of the CO molecules
is monitored and quantified. Methods. Tunable monochromatic VUV light from the
DESIRS beamline of the SOLEIL synchrotron is used in the 7 - 13.6 eV (177 - 91
nm) range to irradiate pure CH4 or layers of CH4 deposited on top of CO ice
samples. The release of species in the gas phase is monitored by quadrupole
mass spectrometry and absolute photodesorption yields of intact CH4 are
deduced. Results. CH4 photodesorbs for photon energies higher than ~9.1 eV
(~136 nm). The photodesorption spectrum follows the absorption spectrum of CH4,
which confirms a desorption mechanism mediated by electronic transitions in the
ice. When it is deposited on top of CO, CH4 desorbs between 8 and 9 eV with a
pattern characteristic of CO absorption, indicating desorption induced by
energy transfer from CO molecules. Conclusions. The photodesorption of CH4 from
the pure ice in various interstellar environments is around 2.0 x 10^-3
molecules per incident photon. Results on CO-induced indirect desorption of CH4
provide useful insights for the generalization of this process to other
molecules co-existing with CO in ice mantles
Indirect Ultraviolet Photodesorption from CO:N2 Binary Ices â An Efficient Grain-Gas Process
Ultraviolet (UV) ice photodesorption is an important non-thermal desorption pathway in many interstellar environments that has been invoked to explain observations of cold molecules in disks, clouds, and cloud cores. Systematic laboratory studies of the photodesorption rates, between 7 and 14 eV, from CO:N2 binary ices, have been performed at the DESIRS vacuum UV beamline of the synchrotron facility SOLEIL. The photodesorption spectral analysis demonstrates that the photodesorption process is indirect, i.e., the desorption is induced by a photon absorption in sub-surface molecular layers, while only surface molecules are actually desorbing. The photodesorption spectra of CO and N2 in binary ices therefore depend on the absorption spectra of the dominant species in the sub-surface ice layer, which implies that the photodesorption efficiency and energy dependence are dramatically different for mixed and layered ices compared with pure ices. In particular, a thin (1-2 ML) N2 ice layer on top of CO will effectively quench CO photodesorption, while enhancing N2 photodesorption by a factor of a few (compared with the pure ices) when the ice is exposed to a typical dark cloud UV field, which may help to explain the different distributions of CO and N2H+ in molecular cloud cores. This indirect photodesorption mechanism may also explain observations of small amounts of complex organics in cold interstellar environments.Astronom
Les effets conjugués de la gestion parcellaire et du contexte paysager et de sa dynamique sur les bioagresseurs et les niveaux de régulation biologique
Ce sĂ©minaire est une restitution des principales avancĂ©es obtenues dans le cadre des projets ANR PEERLESS «viabilitĂ© dâune gestion Ă©cologique renforcĂ©e de la santĂ© des plantes dans les paysages agricoles » (2013-2017) et FRB SEBIOPAG-PHYTO «dĂ©terminants agricoles parcellaires et paysagers des variations de niveaux de rĂ©gulation biologique » (2014-2017). Le sĂ©minaire a rassemblĂ© 60 scientifiques, pour moitiĂ© extĂ©rieure aux unitĂ©s INRA partenaires de ces projets. Il s'est dĂ©roulĂ© Ă Paris Paris les 27-28 novembre 2017
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Initial results from the InSight mission on Mars
NASAâs InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018. It aims to determine the interior structure, composition and thermal state of Mars, as well as constrain present-day seismicity and impact cratering rates. Such information is key to understanding the differentiation and subsequent thermal evolution of Mars, and thus the forces that shape the planetâs surface geology and volatile
processes. Here we report an overview of the first ten months of geophysical observations by InSight. As of 30 September
2019, 174 seismic events have been recorded by the landerâs seismometer, including over 20 events of moment magnitude Mw
= 3â4. The detections thus far are consistent with tectonic origins, with no impact-induced seismicity yet observed, and indi-
cate a seismically active planet. An assessment of these detections suggests that the frequency of global seismic events below
approximately Mw = 3 is similar to that of terrestrial intraplate seismic activity, but there are fewer larger quakes; no quakes
exceeding Mw = 4 have been observed. The landerâs other instrumentsâtwo cameras, atmospheric pressure, temperature and
wind sensors, a magnetometer and a radiometerâhave yielded much more than the intended supporting data for seismometer
noise characterization: magnetic field measurements indicate a local magnetic field that is ten-times stronger than orbital
estimates and meteorological measurements reveal a more dynamic atmosphere than expected, hosting baroclinic and gravity
waves and convective vortices. With the mission due to last for an entire Martian year or longer, these results will be built on by
further measurements by the InSight lander
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