Formation, Habitability, and Detection of Extrasolar Moons
Identifieur interne : 002574 ( Pmc/Curation ); précédent : 002573; suivant : 002575Formation, Habitability, and Detection of Extrasolar Moons
Auteurs : René Heller ; Darren Williams ; David Kipping ; Mary Anne Limbach ; Edwin Turner ; Richard Greenberg ; Takanori Sasaki ; Émeline Bolmont ; Olivier Grasset ; Karen Lewis ; Rory Barnes ; Jorge I. ZuluagaSource :
- Astrobiology [ 1531-1074 ] ; 2014.
Abstract
The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1–0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology. Key Words: Astrobiology—Extrasolar planets—Habitability—Planetary science—Tides. Astrobiology 14, 798–835.
Url:
DOI: 10.1089/ast.2014.1147
PubMed: 25147963
PubMed Central: 4172466
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<front><div type="abstract" xml:lang="en"><title>Abstract</title>
<p>The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1–0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology. Key Words: Astrobiology—Extrasolar planets—Habitability—Planetary science—Tides. Astrobiology 14, 798–835.</p>
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<pmc article-type="review-article"><pmc-comment>The publisher of this article does not allow downloading of the full text in XML form.</pmc-comment>
<front><journal-meta><journal-id journal-id-type="nlm-ta">Astrobiology</journal-id>
<journal-id journal-id-type="iso-abbrev">Astrobiology</journal-id>
<journal-id journal-id-type="publisher-id">ast</journal-id>
<journal-title-group><journal-title>Astrobiology</journal-title>
</journal-title-group>
<issn pub-type="ppub">1531-1074</issn>
<issn pub-type="epub">1557-8070</issn>
<publisher><publisher-name>Mary Ann Liebert, Inc.</publisher-name>
<publisher-loc>140 Huguenot Street, 3rd FloorNew Rochelle, NY 10801USA</publisher-loc>
</publisher>
</journal-meta>
<article-meta><article-id pub-id-type="pmid">25147963</article-id>
<article-id pub-id-type="pmc">4172466</article-id>
<article-id pub-id-type="publisher-id">10.1089/ast.2014.1147</article-id>
<article-id pub-id-type="doi">10.1089/ast.2014.1147</article-id>
<article-categories><subj-group subj-group-type="heading"><subject>Review Article</subject>
</subj-group>
</article-categories>
<title-group><article-title>Formation, Habitability, and Detection of Extrasolar Moons</article-title>
</title-group>
<contrib-group><contrib contrib-type="author" corresp="yes"><name><surname>Heller</surname>
<given-names>René</given-names>
</name>
<xref ref-type="aff" rid="aff1"><sup>1</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Williams</surname>
<given-names>Darren</given-names>
</name>
<xref ref-type="aff" rid="aff2"><sup>2</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Kipping</surname>
<given-names>David</given-names>
</name>
<xref ref-type="aff" rid="aff3"><sup>3</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Limbach</surname>
<given-names>Mary Anne</given-names>
</name>
<xref ref-type="aff" rid="aff4"><sup>4,</sup>
</xref>
<xref ref-type="aff" rid="aff5"><sup>5</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Turner</surname>
<given-names>Edwin</given-names>
</name>
<xref ref-type="aff" rid="aff4"><sup>4,</sup>
</xref>
<xref ref-type="aff" rid="aff6"><sup>6</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Greenberg</surname>
<given-names>Richard</given-names>
</name>
<xref ref-type="aff" rid="aff7"><sup>7</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Sasaki</surname>
<given-names>Takanori</given-names>
</name>
<xref ref-type="aff" rid="aff8"><sup>8</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Bolmont</surname>
<given-names>Émeline</given-names>
</name>
<xref ref-type="aff" rid="aff9"><sup>9,</sup>
</xref>
<xref ref-type="aff" rid="aff10"><sup>10</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Grasset</surname>
<given-names>Olivier</given-names>
</name>
<xref ref-type="aff" rid="aff11"><sup>11</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Lewis</surname>
<given-names>Karen</given-names>
</name>
<xref ref-type="aff" rid="aff12"><sup>12</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Barnes</surname>
<given-names>Rory</given-names>
</name>
<xref ref-type="aff" rid="aff13"><sup>13,</sup>
</xref>
<xref ref-type="aff" rid="aff14"><sup>14</sup>
</xref>
</contrib>
<contrib contrib-type="author"><name><surname>Zuluaga</surname>
<given-names>Jorge I.</given-names>
</name>
<xref ref-type="aff" rid="aff15"><sup>15</sup>
</xref>
</contrib>
<aff id="aff1"><label><sup>1</sup>
</label>
Origins Institute, Department of Physics and Astronomy,<institution>McMaster University</institution>
, Hamilton,<country>Canada</country>
.</aff>
<aff id="aff2"><label><sup>2</sup>
</label>
<institution>The Behrend College School of Science</institution>
, Penn State Erie, Erie, Pennsylvania,<country>USA</country>
.</aff>
<aff id="aff3"><label><sup>3</sup>
</label>
<institution>Harvard-Smithsonian Center for Astrophysics</institution>
, Cambridge, Massachusetts,<country>USA</country>
.</aff>
<aff id="aff4"><label><sup>4</sup>
</label>
Department of Astrophysical Sciences,<institution>Princeton University</institution>
, Princeton, New Jersey,<country>USA</country>
.</aff>
<aff id="aff5"><label><sup>5</sup>
</label>
Department of Mechanical and Aerospace Engineering,<institution>Princeton University</institution>
, Princeton, New Jersey,<country>USA</country>
.</aff>
<aff id="aff6"><label><sup>6</sup>
</label>
The Kavli Institute for the Physics and Mathematics of the Universe,<institution>The University of Tokyo</institution>
, Kashiwa,<country>Japan</country>
.</aff>
<aff id="aff7"><label><sup>7</sup>
</label>
Lunar and Planetary Laboratory,<institution>University of Arizona</institution>
, Tucson, Arizona,<country>USA</country>
.</aff>
<aff id="aff8"><label><sup>8</sup>
</label>
Department of Astronomy,<institution>Kyoto University</institution>
, Kyoto,<country>Japan</country>
.</aff>
<aff id="aff9"><label><sup>9</sup>
</label>
<institution>Université de Bordeaux</institution>
, LAB, UMR 5804, Floirac,<country>France</country>
.</aff>
<aff id="aff10"><label><sup>10</sup>
</label>
<institution>CNRS</institution>
, LAB, UMR 5804, Floirac,<country>France</country>
.</aff>
<aff id="aff11"><label><sup>11</sup>
</label>
Planetology and Geodynamics,<institution>University of Nantes</institution>
, CNRS, Nantes,<country>France</country>
.</aff>
<aff id="aff12"><label><sup>12</sup>
</label>
Earth and Planetary Sciences,<institution>Tokyo Institute of Technology</institution>
, Tokyo,<country>Japan</country>
.</aff>
<aff id="aff13"><label><sup>13</sup>
</label>
Astronomy Department,<institution>University of Washington</institution>
, Seattle, Washington,<country>USA</country>
.</aff>
<aff id="aff14"><label><sup>14</sup>
</label>
<institution>NASA Astrobiology Institute—Virtual Planetary Laboratory Lead Team</institution>
,<country>USA</country>
.</aff>
<aff id="aff15"><label><sup>15</sup>
</label>
FACom—Instituto de Física—FCEN,<institution>Universidad de Antioquia</institution>
, Medellín,<country>Colombia</country>
.</aff>
</contrib-group>
<author-notes><corresp><addr-line>Address correspondence to:</addr-line>
<addr-line><italic>René Heller</italic>
</addr-line>
<addr-line><italic>Origins Institute</italic>
</addr-line>
<addr-line><italic>Department of Physics and Astronomy</italic>
</addr-line>
<institution><italic>McMaster University</italic>
</institution>
<addr-line><italic>Hamilton, ON L8S 4M1</italic>
</addr-line>
<country>Canada</country>
<break></break>
<italic>E-mail:</italic>
<email xlink:href="mailto:rheller@physics.mcmaster.ca">rheller@physics.mcmaster.ca</email>
</corresp>
</author-notes>
<pub-date pub-type="ppub"><day>01</day>
<month>9</month>
<year>2014</year>
<pmc-comment>string-date: September 2014</pmc-comment>
</pub-date>
<volume>14</volume>
<issue>9</issue>
<fpage>798</fpage>
<lpage>835</lpage>
<history><date date-type="received"><day>20</day>
<month>1</month>
<year>2014</year>
<pmc-comment>string-date: Submitted 20 January 2014</pmc-comment>
</date>
<date date-type="accepted"><day>05</day>
<month>6</month>
<year>2014</year>
<pmc-comment>string-date: Accepted 5 June 2014</pmc-comment>
</date>
</history>
<permissions><copyright-statement>Copyright 2014, Mary Ann Liebert, Inc.</copyright-statement>
<copyright-year>2014</copyright-year>
</permissions>
<self-uri content-type="pdf" xlink:type="simple" xlink:href="ast.2014.1147.pdf"></self-uri>
<abstract><title>Abstract</title>
<p>The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1–0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology. Key Words: Astrobiology—Extrasolar planets—Habitability—Planetary science—Tides. Astrobiology 14, 798–835.</p>
</abstract>
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