Detailed Abundances of Stars with Small Planets Discovered by Kepler I: The First Sample
We present newly derived stellar parameters and the detailed abundances of 19 elements of seven stars with small planets discovered by NASA's Kepler Mission. Each star save one has at least one planet with a radius
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| creator | Schuler, Simon C Vaz, Zachary A Orlando J Katime Santrich Cunha, Katia Smith, Verne V King, Jeremy R Teske, Johanna K Ghezzi, Luan Howell, Steve B Isaacson, Howard |
| description | We present newly derived stellar parameters and the detailed abundances of 19 elements of seven stars with small planets discovered by NASA's Kepler Mission. Each star save one has at least one planet with a radius |
| doi_str_mv | 10.48550/arxiv.1511.00934 |
| format | Article |
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Each star save one has at least one planet with a radius <= 1.6 R_Earth, suggesting a primarily rocky composition. The stellar parameters and abundances are derived from high signal-to-noise ratio, high-resolution echelle spectroscopy obtained with the 10-m Keck I telescope and HIRES spectrometer using standard spectroscopic techniques. The metallicities of the seven stars range from -0.32 dex to +0.13 dex, with an average metallicity that is subsolar, supporting previous suggestions that, unlike Jupiter-type giant planets, small planets do not form preferentially around metal-rich stars. The abundances of elements other than iron are in line with a population of Galactic disk stars, and despite our modest sample size, we find hints that the compositions of stars with small planets are similar to stars without known planets and with Neptune-size planets, but not to those of stars with giant planets. This suggests that the formation of small planets does not require exceptional host-star compositions and that small planets may be ubiquitous in the Galaxy. We compare our derived abundances (which have typical uncertainties of <= 0.04 dex) to the condensation temperature of the elements; a correlation between the two has been suggested as a possible signature of rocky planet formation. None of the stars demonstrate the putative rocky planet signature, despite at least three of the stars having rocky planets estimated to contain enough refractory material to produce the signature, if real. More detailed abundance analyses of stars known to host small planets are needed to verify our results and place ever more stringent constraints on planet formation models.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1511.00934</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Abundance ; Condensates ; Constraint modelling ; Extrasolar planets ; Galactic disk ; Galaxies ; Jupiter ; Kepler mission (NASA) ; Metallicity ; Neptune ; Parameters ; Physics - Solar and Stellar Astrophysics ; Planet detection ; Planet formation ; Planetary composition ; Refractory materials ; Stars ; Terrestrial planets</subject><ispartof>arXiv.org, 2015-11</ispartof><rights>2015. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,781,785,886,27930</link.rule.ids><backlink>$$Uhttps://doi.org/10.1088/0004-637X/815/1/5$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1511.00934$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Schuler, Simon C</creatorcontrib><creatorcontrib>Vaz, Zachary A</creatorcontrib><creatorcontrib>Orlando J Katime Santrich</creatorcontrib><creatorcontrib>Cunha, Katia</creatorcontrib><creatorcontrib>Smith, Verne V</creatorcontrib><creatorcontrib>King, Jeremy R</creatorcontrib><creatorcontrib>Teske, Johanna K</creatorcontrib><creatorcontrib>Ghezzi, Luan</creatorcontrib><creatorcontrib>Howell, Steve B</creatorcontrib><creatorcontrib>Isaacson, Howard</creatorcontrib><title>Detailed Abundances of Stars with Small Planets Discovered by Kepler I: The First Sample</title><title>arXiv.org</title><description>We present newly derived stellar parameters and the detailed abundances of 19 elements of seven stars with small planets discovered by NASA's Kepler Mission. Each star save one has at least one planet with a radius <= 1.6 R_Earth, suggesting a primarily rocky composition. The stellar parameters and abundances are derived from high signal-to-noise ratio, high-resolution echelle spectroscopy obtained with the 10-m Keck I telescope and HIRES spectrometer using standard spectroscopic techniques. The metallicities of the seven stars range from -0.32 dex to +0.13 dex, with an average metallicity that is subsolar, supporting previous suggestions that, unlike Jupiter-type giant planets, small planets do not form preferentially around metal-rich stars. The abundances of elements other than iron are in line with a population of Galactic disk stars, and despite our modest sample size, we find hints that the compositions of stars with small planets are similar to stars without known planets and with Neptune-size planets, but not to those of stars with giant planets. This suggests that the formation of small planets does not require exceptional host-star compositions and that small planets may be ubiquitous in the Galaxy. We compare our derived abundances (which have typical uncertainties of <= 0.04 dex) to the condensation temperature of the elements; a correlation between the two has been suggested as a possible signature of rocky planet formation. None of the stars demonstrate the putative rocky planet signature, despite at least three of the stars having rocky planets estimated to contain enough refractory material to produce the signature, if real. More detailed abundance analyses of stars known to host small planets are needed to verify our results and place ever more stringent constraints on planet formation models.</description><subject>Abundance</subject><subject>Condensates</subject><subject>Constraint modelling</subject><subject>Extrasolar planets</subject><subject>Galactic disk</subject><subject>Galaxies</subject><subject>Jupiter</subject><subject>Kepler mission (NASA)</subject><subject>Metallicity</subject><subject>Neptune</subject><subject>Parameters</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planet detection</subject><subject>Planet formation</subject><subject>Planetary composition</subject><subject>Refractory materials</subject><subject>Stars</subject><subject>Terrestrial planets</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj01Lw0AYhBdBsNT-AE8ueE7dr3d34620VosFhfbgLbxJNjQlX-6m1f57Y-tpYJgZ5iHkjrOpsgDsEf1PeZxy4HzKWCzVFRkJKXlklRA3ZBLCnjEmtBEAckQ-F67HsnI5naWHJscmc4G2Bd306AP9Lvsd3dRYVfSjwsb1gS7KkLVH54dGeqJvrqucp6snut05uix96OkG68G8JdcFVsFN_nVMtsvn7fw1Wr-_rOazdYQgTGSZVk7leaYALGRaAONFYbgSwF2hYlRax0zEAhU4jgUA2gxSHhuRSqFjOSb3l9kzdtL5skZ_Sv7wkzP-kHi4JDrffh1c6JN9e_DN8CkRzEqrDTNG_gI0DFsV</recordid><startdate>20151103</startdate><enddate>20151103</enddate><creator>Schuler, Simon C</creator><creator>Vaz, Zachary A</creator><creator>Orlando J Katime Santrich</creator><creator>Cunha, Katia</creator><creator>Smith, Verne V</creator><creator>King, Jeremy R</creator><creator>Teske, Johanna K</creator><creator>Ghezzi, Luan</creator><creator>Howell, Steve B</creator><creator>Isaacson, Howard</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20151103</creationdate><title>Detailed Abundances of Stars with Small Planets Discovered by Kepler I: The First Sample</title><author>Schuler, Simon C ; Vaz, Zachary A ; Orlando J Katime Santrich ; Cunha, Katia ; Smith, Verne V ; King, Jeremy R ; Teske, Johanna K ; Ghezzi, Luan ; Howell, Steve B ; Isaacson, Howard</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a527-8064e4ddc45585c62501ff714251ef49a46690292a45e1af55a8c5b1972b32693</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Abundance</topic><topic>Condensates</topic><topic>Constraint modelling</topic><topic>Extrasolar planets</topic><topic>Galactic disk</topic><topic>Galaxies</topic><topic>Jupiter</topic><topic>Kepler mission (NASA)</topic><topic>Metallicity</topic><topic>Neptune</topic><topic>Parameters</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planet detection</topic><topic>Planet formation</topic><topic>Planetary composition</topic><topic>Refractory materials</topic><topic>Stars</topic><topic>Terrestrial planets</topic><toplevel>online_resources</toplevel><creatorcontrib>Schuler, Simon C</creatorcontrib><creatorcontrib>Vaz, Zachary A</creatorcontrib><creatorcontrib>Orlando J Katime Santrich</creatorcontrib><creatorcontrib>Cunha, Katia</creatorcontrib><creatorcontrib>Smith, Verne V</creatorcontrib><creatorcontrib>King, Jeremy R</creatorcontrib><creatorcontrib>Teske, Johanna K</creatorcontrib><creatorcontrib>Ghezzi, Luan</creatorcontrib><creatorcontrib>Howell, Steve B</creatorcontrib><creatorcontrib>Isaacson, Howard</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>SciTech Premium Collection (Proquest) (PQ_SDU_P3)</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Access via ProQuest (Open Access)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Schuler, Simon C</au><au>Vaz, Zachary A</au><au>Orlando J Katime Santrich</au><au>Cunha, Katia</au><au>Smith, Verne V</au><au>King, Jeremy R</au><au>Teske, Johanna K</au><au>Ghezzi, Luan</au><au>Howell, Steve B</au><au>Isaacson, Howard</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Detailed Abundances of Stars with Small Planets Discovered by Kepler I: The First Sample</atitle><jtitle>arXiv.org</jtitle><date>2015-11-03</date><risdate>2015</risdate><eissn>2331-8422</eissn><abstract>We present newly derived stellar parameters and the detailed abundances of 19 elements of seven stars with small planets discovered by NASA's Kepler Mission. Each star save one has at least one planet with a radius <= 1.6 R_Earth, suggesting a primarily rocky composition. The stellar parameters and abundances are derived from high signal-to-noise ratio, high-resolution echelle spectroscopy obtained with the 10-m Keck I telescope and HIRES spectrometer using standard spectroscopic techniques. The metallicities of the seven stars range from -0.32 dex to +0.13 dex, with an average metallicity that is subsolar, supporting previous suggestions that, unlike Jupiter-type giant planets, small planets do not form preferentially around metal-rich stars. The abundances of elements other than iron are in line with a population of Galactic disk stars, and despite our modest sample size, we find hints that the compositions of stars with small planets are similar to stars without known planets and with Neptune-size planets, but not to those of stars with giant planets. This suggests that the formation of small planets does not require exceptional host-star compositions and that small planets may be ubiquitous in the Galaxy. We compare our derived abundances (which have typical uncertainties of <= 0.04 dex) to the condensation temperature of the elements; a correlation between the two has been suggested as a possible signature of rocky planet formation. None of the stars demonstrate the putative rocky planet signature, despite at least three of the stars having rocky planets estimated to contain enough refractory material to produce the signature, if real. More detailed abundance analyses of stars known to host small planets are needed to verify our results and place ever more stringent constraints on planet formation models.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1511.00934</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Abundance Condensates Constraint modelling Extrasolar planets Galactic disk Galaxies Jupiter Kepler mission (NASA) Metallicity Neptune Parameters Physics - Solar and Stellar Astrophysics Planet detection Planet formation Planetary composition Refractory materials Stars Terrestrial planets |
| title | Detailed Abundances of Stars with Small Planets Discovered by Kepler I: The First Sample |
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