What Is the Total Deuterium Abundance in the Local Galactic Disk?

Linsky, Jeffrey L.; Draine, B. T.; Moos, H. W.; Jenkins, Edward B.; Wood, Brian E.; Oliveira, Cristina; Blair, William P.; Friedman, S. D.; Gry, C.; Knauth, D. C.; Kruk, J. W.; Lacour, S.; Lehner, N.; Redfield, Seth; Shull, J. M.; Sonneborn, G.; Williger, G. M.

doi:10.1086/505556

Cited by 308 publications

(498 citation statements)

References 116 publications

(166 reference statements)

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“…(Linsky et al 2006). These ratios are consistent with 0.018-0.08 from a study of DNC and HNC towards UCH II regions, which are an order of magnitude lower than the high-mass starless core candidates (HMSCs; Fontani et al 2014).…”

Section: D/hsupporting

confidence: 88%

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Wang

Zhang

et al. 2017

Mon. Not. R. Astron. Soc.

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We present spectral line mapping observations towards four massive star-forming regionsCepheus A, DR21S, S76E and G34.26+0.15 -with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 14 0, 14 -13 0, 13 ) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C 3 H 2 and NH 2 D show enhancement in shocked regions, as suggested by the evidence of SiO and/or SO emission. The column density and rotational temperature of CH 3 CN were estimated with the rotational diagram method for all four sources. Isotope abundance ratios of 12 C/ 13 C were derived using HC 3 N and its 13 C isotopologue, which were around 40 in all four massive star-forming regions and slightly lower than the local interstellar value (∼65). The 14 N/ 15 N and 16 O/ 18 O abundance ratios in these sources were also derived using the double isotopic method, which were slightly lower than in the local interstellar medium. Except for Cep A, the 33 S/ 34 S ratios in the other three targets were derived, which were similar to that in the local interstellar medium. The column density ratios of N(DCN)/N(HCN) and N(DCO + )/N(HCO + ) in these sources were more than two orders of magnitude higher than the elemental [D]/[H] ratio, which is 1.5 × 10 −5 . Our results show that the later stage sources, G34.26+0.15 in particular, present more molecular species than earlier stage sources. Evidence of shock activity is seen in all stages studied.

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Section: D/hsupporting

confidence: 88%

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Wang

Zhang

et al. 2017

Mon. Not. R. Astron. Soc.

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“…Copyright © 2013 Elsevier 1.0 × 10 −2 and 1.0 × 10 −3 respectively. This is an enrichment of 2-3 orders of magnitude relative to the D/H ratio of protosolar hydrogen, 2.1 × 10 −6 , or the local interstellar medium, 1.6 × 10 −6 (Linsky et al 2006). These values may be considered as upper and lower limits of the D/H ratio in water in our solar system, taking into account the possibility of isotopic exchange between water and hydrogen.…”

Section: Water and D/hmentioning

confidence: 95%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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“…(1) Cyburt et al (2008); (2) Pettini et al (2008); (3) Geiss & Gloeckler (1998); (4) Linsky et al (2006); (5) Hébrard et al (2005); (6) Prodanović et al (2009); (7) Bania et al (2002); (8) Gloeckler & Geiss (1996); (9) Peimbert et al (2007); (10) Steigman (2007); (11) Asplund et al (2009). can not be reproduced by the models, independently of how many low-mass stars burn their 3 He on the RGB.…”

Section: Referencesmentioning

confidence: 98%

“…The FUSE satellite has measured the deteurium abundance along the lines of sight to several stars in the Local Bubble as well as beyond it, up to 1-2 kpc away. The dispersion (by a factor of 3) which has been found in the measurements (Linsky et al 2006) makes it hard to interpret the data in the context of standard GCE models. It has been suggested (Hébrard et al 2005, Linsky et al 2006 that either the lowest (see also text by G. Hébrard, this volume) or the highest (see also text by J. Linsky, this volume) observed abundances are indicative of the actual value of the deuterium abundance in the local ISM (LISM).…”

Section: Deuteriummentioning

confidence: 99%

“…The dispersion (by a factor of 3) which has been found in the measurements (Linsky et al 2006) makes it hard to interpret the data in the context of standard GCE models. It has been suggested (Hébrard et al 2005, Linsky et al 2006 that either the lowest (see also text by G. Hébrard, this volume) or the highest (see also text by J. Linsky, this volume) observed abundances are indicative of the actual value of the deuterium abundance in the local ISM (LISM). However, neither of these values can be reproduced by GCE models in agreement with all the major observational constraints for the solar neighbourhood (Romano et al 2006).…”

Section: Deuteriummentioning

confidence: 99%

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Galactic evolution of D, ³He and ⁴He

Romano

2009

Proc. IAU

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Abstract. The uncertainties which still plague our understanding of the evolution of the light nuclides D, 3 He and 4 He in the Galaxy are described. Measurements of the local abundance of deuterium range over a factor of 3. The observed dispersion can be reconciled with the predictions on deuterium evolution from standard Galactic chemical evolution models, if the true local abundance of deuterium proves to be high, but not too high, and lower observed values are due to depletion onto dust grains. The nearly constancy of the 3 He abundance with both time and position within the Galaxy implies a negligible production of this element in stars, at variance with predictions from standard stellar models which, however, do agree with the (few) measurements of 3 He in planetary nebulae. Thermohaline mixing, inhibited by magnetic fields in a small fraction of low-mass stars, could in principle explain the complexity of the overall scenario. However, complete grids of stellar yields taking this mechanism into account are not available for use in chemical evolution models yet. Much effort has been devoted to unravel the origin of the extreme helium-rich stars which seem to inhabit the most massive Galactic globular clusters. Yet, the issue of 4 He evolution is far from being fully settled even in the disc of the Milky Way.

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What Is the Total Deuterium Abundance in the Local Galactic Disk?

Cited by 308 publications

References 116 publications

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

Galactic evolution of D, ³He and ⁴He

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What Is the Total Deuterium Abundance in the Local Galactic Disk?

Cited by 308 publications

References 116 publications

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

Galactic evolution of D, 3He and 4He

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Product

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Galactic evolution of D, ³He and ⁴He