Large-scale dissociation of molecular gas in galaxies by newly formed stars

R. J. Allen; P. D. Atherton; R. P.J. Tilanus

doi:10.1038/319296a0

Large-scale dissociation of molecular gas in galaxies by newly formed stars

R. J. Allen, P. D. Atherton, R. P.J. Tilanus

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Abstract

Molecular hydrogen is thought to form from atomic hydrogen on the surface of dust grains in the interstellar medium, and to be dissociated primarily by ultraviolet radiation from hot stars¹. This process has been modelled on the 1 pc length scale for the case of dense interstellar clouds² and near newly formed ionizing stars³. Observational evidence that molecular hydrogen is indeed dissociated in shells around young OB stars in the Galaxy has been presented recently^4-6. We suggest here that the same dissociation process occurs on the kpc scale in active star-forming regions of some galaxies, and that this dissociation may strongly affect the observed morphology of atomic hydrogen in spiral arms.

Original language	English (US)
Pages (from-to)	296-298
Number of pages	3
Journal	Nature
Volume	319
Issue number	6051
DOIs	https://doi.org/10.1038/319296a0
State	Published - 1986
Externally published	Yes

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@article{b117b26789d04e0088871094ed215595,

title = "Large-scale dissociation of molecular gas in galaxies by newly formed stars",

abstract = "Molecular hydrogen is thought to form from atomic hydrogen on the surface of dust grains in the interstellar medium, and to be dissociated primarily by ultraviolet radiation from hot stars1. This process has been modelled on the 1 pc length scale for the case of dense interstellar clouds2 and near newly formed ionizing stars3. Observational evidence that molecular hydrogen is indeed dissociated in shells around young OB stars in the Galaxy has been presented recently4-6. We suggest here that the same dissociation process occurs on the kpc scale in active star-forming regions of some galaxies, and that this dissociation may strongly affect the observed morphology of atomic hydrogen in spiral arms.",

author = "Allen, {R. J.} and Atherton, {P. D.} and Tilanus, {R. P.J.}",

year = "1986",

doi = "10.1038/319296a0",

language = "English (US)",

volume = "319",

pages = "296--298",

journal = "Nature",

issn = "0028-0836",

publisher = "Nature Research",

number = "6051",

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TY - JOUR

T1 - Large-scale dissociation of molecular gas in galaxies by newly formed stars

AU - Allen, R. J.

AU - Atherton, P. D.

AU - Tilanus, R. P.J.

PY - 1986

Y1 - 1986

N2 - Molecular hydrogen is thought to form from atomic hydrogen on the surface of dust grains in the interstellar medium, and to be dissociated primarily by ultraviolet radiation from hot stars1. This process has been modelled on the 1 pc length scale for the case of dense interstellar clouds2 and near newly formed ionizing stars3. Observational evidence that molecular hydrogen is indeed dissociated in shells around young OB stars in the Galaxy has been presented recently4-6. We suggest here that the same dissociation process occurs on the kpc scale in active star-forming regions of some galaxies, and that this dissociation may strongly affect the observed morphology of atomic hydrogen in spiral arms.

AB - Molecular hydrogen is thought to form from atomic hydrogen on the surface of dust grains in the interstellar medium, and to be dissociated primarily by ultraviolet radiation from hot stars1. This process has been modelled on the 1 pc length scale for the case of dense interstellar clouds2 and near newly formed ionizing stars3. Observational evidence that molecular hydrogen is indeed dissociated in shells around young OB stars in the Galaxy has been presented recently4-6. We suggest here that the same dissociation process occurs on the kpc scale in active star-forming regions of some galaxies, and that this dissociation may strongly affect the observed morphology of atomic hydrogen in spiral arms.

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DO - 10.1038/319296a0

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VL - 319

SP - 296

EP - 298

JO - Nature

JF - Nature

IS - 6051

ER -

Large-scale dissociation of molecular gas in galaxies by newly formed stars

Abstract

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