A reappraisal of the habitability of planets around M dwarf stars

Jill C. Tarter, Peter R. Backus, Rocco L. Mancinelli, Jonathan M. Aurnou, Dana E. Backman, Gibor S. Basri, Alan P. Boss, Andrew Clarke, Drake Deming, Laurance R. Doyle, Eric D. Feigelson, Friedmann Freund, David H. Grinspoon, Robert M. Haberle, Steven A. Hauck, Martin J. Heath, Todd J. Henry, Jeffery L. Hollingsworth, Manoj M. Joshi, Steven KilstonMichael C. Liu, Eric Meikle, I. Neill Reid, Lynn J. Rothschild, John Scalo, Antigona Segura, Carol M. Tang, James M. Tiedje, Margaret C. Turnbull, Lucianne M. Walkowicz, Arthur L. Weber, Richard E. Young

Research output: Contribution to journalArticle

183 Citations (Scopus)

Abstract

Stable, hydrogen-burning, M dwarf stars make up about 75% of all stars in the Galaxy. They are extremely long-lived, and because they are much smaller in mass than the Sun (between 0.5 and 0.08 MSun), their temperature and stellar luminosity are low and peaked in the red. We have re-examined what is known at present about the potential for a terrestrial planet forming within, or migrating into, the classic liquid-surface-water habitable zone close to an M dwarf star. Observations of protoplanetary disks suggest that planet-building materials are common around M dwarfs, but N-body simulations differ in their estimations of the likelihood of potentially habitable, wet planets that reside within their habitable zones, which are only about one-fifth to 1/50th of the width of that for a G star. Particularly in light of the claimed detection of the planets with masses as small as 5.5 and 7.5/Earth orbiting M stars, there seems no reason to exclude the possibility of terrestrial planets. Tidally locked synchronous rotation within the narrow habitable zone does not necessarily lead to atmospheric collapse, and active stellar flaring may not be as much of an evolutionarily disadvantageous factor as has previously been supposed. We conclude that M dwarf stars may indeed be viable hosts for planets on which the origin and evolution of life can occur. A number of planetary processes such as cessation of geother mal activity or thermal and nonthermal atmospheric loss processes may limit the duration of planetary habitability to periods far shorter than the extreme lifetime of the M dwarf star. Nevertheless, it makes sense to include M dwarf stars in programs that seek to find habitable worlds and evidence of life. This paper presents the summary conclusions of an interdisciplinary workshop (http://mstars.seti.org) sponsored by the NASA Astrobiology Institute and convened at the SETI Institute.

Original languageEnglish (US)
Pages (from-to)30-65
Number of pages36
JournalAstrobiology
Volume7
Issue number1
DOIs
StatePublished - Feb 1 2007

Fingerprint

habitability
Planets
dwarf stars
M stars
planets
planet
hydrogen
surface water
terrestrial planets
heat
duration
liquids
Exobiology
Galaxies
Project SETI
United States National Aeronautics and Space Administration
G stars
stellar luminosity
exobiology
temperature

All Science Journal Classification (ASJC) codes

  • Agricultural and Biological Sciences (miscellaneous)
  • Space and Planetary Science

Cite this

Tarter, J. C., Backus, P. R., Mancinelli, R. L., Aurnou, J. M., Backman, D. E., Basri, G. S., ... Young, R. E. (2007). A reappraisal of the habitability of planets around M dwarf stars. Astrobiology, 7(1), 30-65. https://doi.org/10.1089/ast.2006.0124
Tarter, Jill C. ; Backus, Peter R. ; Mancinelli, Rocco L. ; Aurnou, Jonathan M. ; Backman, Dana E. ; Basri, Gibor S. ; Boss, Alan P. ; Clarke, Andrew ; Deming, Drake ; Doyle, Laurance R. ; Feigelson, Eric D. ; Freund, Friedmann ; Grinspoon, David H. ; Haberle, Robert M. ; Hauck, Steven A. ; Heath, Martin J. ; Henry, Todd J. ; Hollingsworth, Jeffery L. ; Joshi, Manoj M. ; Kilston, Steven ; Liu, Michael C. ; Meikle, Eric ; Reid, I. Neill ; Rothschild, Lynn J. ; Scalo, John ; Segura, Antigona ; Tang, Carol M. ; Tiedje, James M. ; Turnbull, Margaret C. ; Walkowicz, Lucianne M. ; Weber, Arthur L. ; Young, Richard E. / A reappraisal of the habitability of planets around M dwarf stars. In: Astrobiology. 2007 ; Vol. 7, No. 1. pp. 30-65.
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Tarter, JC, Backus, PR, Mancinelli, RL, Aurnou, JM, Backman, DE, Basri, GS, Boss, AP, Clarke, A, Deming, D, Doyle, LR, Feigelson, ED, Freund, F, Grinspoon, DH, Haberle, RM, Hauck, SA, Heath, MJ, Henry, TJ, Hollingsworth, JL, Joshi, MM, Kilston, S, Liu, MC, Meikle, E, Reid, IN, Rothschild, LJ, Scalo, J, Segura, A, Tang, CM, Tiedje, JM, Turnbull, MC, Walkowicz, LM, Weber, AL & Young, RE 2007, 'A reappraisal of the habitability of planets around M dwarf stars', Astrobiology, vol. 7, no. 1, pp. 30-65. https://doi.org/10.1089/ast.2006.0124

A reappraisal of the habitability of planets around M dwarf stars. / Tarter, Jill C.; Backus, Peter R.; Mancinelli, Rocco L.; Aurnou, Jonathan M.; Backman, Dana E.; Basri, Gibor S.; Boss, Alan P.; Clarke, Andrew; Deming, Drake; Doyle, Laurance R.; Feigelson, Eric D.; Freund, Friedmann; Grinspoon, David H.; Haberle, Robert M.; Hauck, Steven A.; Heath, Martin J.; Henry, Todd J.; Hollingsworth, Jeffery L.; Joshi, Manoj M.; Kilston, Steven; Liu, Michael C.; Meikle, Eric; Reid, I. Neill; Rothschild, Lynn J.; Scalo, John; Segura, Antigona; Tang, Carol M.; Tiedje, James M.; Turnbull, Margaret C.; Walkowicz, Lucianne M.; Weber, Arthur L.; Young, Richard E.

In: Astrobiology, Vol. 7, No. 1, 01.02.2007, p. 30-65.

Research output: Contribution to journalArticle

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AU - Tarter, Jill C.

AU - Backus, Peter R.

AU - Mancinelli, Rocco L.

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AU - Basri, Gibor S.

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AU - Hauck, Steven A.

AU - Heath, Martin J.

AU - Henry, Todd J.

AU - Hollingsworth, Jeffery L.

AU - Joshi, Manoj M.

AU - Kilston, Steven

AU - Liu, Michael C.

AU - Meikle, Eric

AU - Reid, I. Neill

AU - Rothschild, Lynn J.

AU - Scalo, John

AU - Segura, Antigona

AU - Tang, Carol M.

AU - Tiedje, James M.

AU - Turnbull, Margaret C.

AU - Walkowicz, Lucianne M.

AU - Weber, Arthur L.

AU - Young, Richard E.

PY - 2007/2/1

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N2 - Stable, hydrogen-burning, M dwarf stars make up about 75% of all stars in the Galaxy. They are extremely long-lived, and because they are much smaller in mass than the Sun (between 0.5 and 0.08 MSun), their temperature and stellar luminosity are low and peaked in the red. We have re-examined what is known at present about the potential for a terrestrial planet forming within, or migrating into, the classic liquid-surface-water habitable zone close to an M dwarf star. Observations of protoplanetary disks suggest that planet-building materials are common around M dwarfs, but N-body simulations differ in their estimations of the likelihood of potentially habitable, wet planets that reside within their habitable zones, which are only about one-fifth to 1/50th of the width of that for a G star. Particularly in light of the claimed detection of the planets with masses as small as 5.5 and 7.5/Earth orbiting M stars, there seems no reason to exclude the possibility of terrestrial planets. Tidally locked synchronous rotation within the narrow habitable zone does not necessarily lead to atmospheric collapse, and active stellar flaring may not be as much of an evolutionarily disadvantageous factor as has previously been supposed. We conclude that M dwarf stars may indeed be viable hosts for planets on which the origin and evolution of life can occur. A number of planetary processes such as cessation of geother mal activity or thermal and nonthermal atmospheric loss processes may limit the duration of planetary habitability to periods far shorter than the extreme lifetime of the M dwarf star. Nevertheless, it makes sense to include M dwarf stars in programs that seek to find habitable worlds and evidence of life. This paper presents the summary conclusions of an interdisciplinary workshop (http://mstars.seti.org) sponsored by the NASA Astrobiology Institute and convened at the SETI Institute.

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Tarter JC, Backus PR, Mancinelli RL, Aurnou JM, Backman DE, Basri GS et al. A reappraisal of the habitability of planets around M dwarf stars. Astrobiology. 2007 Feb 1;7(1):30-65. https://doi.org/10.1089/ast.2006.0124