Probing the atmosphere of HD189733b with the Na i and K i lines
ABSTRACT High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmo...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2020-10, Vol.498 (1), p.1023-1033 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Keles, E Kitzmann, D Mallonn, M Alexoudi, X Fossati, L Pino, L Seidel, J V Carroll, T A Steffen, M Ilyin, I Poppenhäger, K Strassmeier, K G von Essen, C Nascimbeni, V Turner, J D |
| description | ABSTRACT
High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmospheric K i absorption on HD189733b with the aim to compare the resolved K i line and previously obtained high-resolution Na i-D line observations with synthetic transmission spectra. The line profiles suggest atmospheric processes leading to a line broadening of the order of ∼10 km/s for the Na i-D lines and only a few km/s for the K i line. The investigation hints that either the atmosphere of HD189733b lacks a significant amount of K i or the alkali lines probe different atmospheric regions with different temperature, which could explain the differences we see in the resolved absorption lines. |
| doi_str_mv | 10.1093/mnras/staa2435 |
| format | Article |
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High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmospheric K i absorption on HD189733b with the aim to compare the resolved K i line and previously obtained high-resolution Na i-D line observations with synthetic transmission spectra. The line profiles suggest atmospheric processes leading to a line broadening of the order of ∼10 km/s for the Na i-D lines and only a few km/s for the K i line. The investigation hints that either the atmosphere of HD189733b lacks a significant amount of K i or the alkali lines probe different atmospheric regions with different temperature, which could explain the differences we see in the resolved absorption lines.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/staa2435</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2020-10, Vol.498 (1), p.1023-1033</ispartof><rights>2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2020</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c2285-b3a1f17314260b0497b436fe03e24655d38e74a76f6caba96f16aa1926a7e9513</citedby><cites>FETCH-LOGICAL-c2285-b3a1f17314260b0497b436fe03e24655d38e74a76f6caba96f16aa1926a7e9513</cites><orcidid>0000-0003-1231-2194 ; 0000-0002-7990-9596 ; 0000-0001-9770-1214 ; 0000-0003-4269-3311</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1603,27922,27923</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/staa2435$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Keles, E</creatorcontrib><creatorcontrib>Kitzmann, D</creatorcontrib><creatorcontrib>Mallonn, M</creatorcontrib><creatorcontrib>Alexoudi, X</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Pino, L</creatorcontrib><creatorcontrib>Seidel, J V</creatorcontrib><creatorcontrib>Carroll, T A</creatorcontrib><creatorcontrib>Steffen, M</creatorcontrib><creatorcontrib>Ilyin, I</creatorcontrib><creatorcontrib>Poppenhäger, K</creatorcontrib><creatorcontrib>Strassmeier, K G</creatorcontrib><creatorcontrib>von Essen, C</creatorcontrib><creatorcontrib>Nascimbeni, V</creatorcontrib><creatorcontrib>Turner, J D</creatorcontrib><title>Probing the atmosphere of HD189733b with the Na i and K i lines</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmospheric K i absorption on HD189733b with the aim to compare the resolved K i line and previously obtained high-resolution Na i-D line observations with synthetic transmission spectra. The line profiles suggest atmospheric processes leading to a line broadening of the order of ∼10 km/s for the Na i-D lines and only a few km/s for the K i line. The investigation hints that either the atmosphere of HD189733b lacks a significant amount of K i or the alkali lines probe different atmospheric regions with different temperature, which could explain the differences we see in the resolved absorption lines.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNqFkD1PwzAURS0EEqWwMntlSOvn5494RAVaRAUMMEcvqU2C2qSygxAbK3-TXwKkMDPdO9xzh8PYKYgJCIfTTRspTVNPJBXqPTYCNDqTzph9NhICdZZbgEN2lNKzEEKhNCM2u49d2bRPvK89p37TpW3to-dd4IsLyJ1FLPlr09fD4JY-3z8aTu2K3wxt3bQ-HbODQOvkT35zzB6vLh9mi2x5N7-enS-zSspcZyUSBLAIShpRCuVsqdAEL9BLZbReYe6tImuCqagkZwIYInDSkPVOA47ZZPdbxS6l6EOxjc2G4lsBovhRUAwKij8F38DZDuhetv9tvwD71F6B</recordid><startdate>20201011</startdate><enddate>20201011</enddate><creator>Keles, E</creator><creator>Kitzmann, D</creator><creator>Mallonn, M</creator><creator>Alexoudi, X</creator><creator>Fossati, L</creator><creator>Pino, L</creator><creator>Seidel, J V</creator><creator>Carroll, T A</creator><creator>Steffen, M</creator><creator>Ilyin, I</creator><creator>Poppenhäger, K</creator><creator>Strassmeier, K G</creator><creator>von Essen, C</creator><creator>Nascimbeni, V</creator><creator>Turner, J D</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0003-1231-2194</orcidid><orcidid>https://orcid.org/0000-0002-7990-9596</orcidid><orcidid>https://orcid.org/0000-0001-9770-1214</orcidid><orcidid>https://orcid.org/0000-0003-4269-3311</orcidid></search><sort><creationdate>20201011</creationdate><title>Probing the atmosphere of HD189733b with the Na i and K i lines</title><author>Keles, E ; Kitzmann, D ; Mallonn, M ; Alexoudi, X ; Fossati, L ; Pino, L ; Seidel, J V ; Carroll, T A ; Steffen, M ; Ilyin, I ; Poppenhäger, K ; Strassmeier, K G ; von Essen, C ; Nascimbeni, V ; Turner, J D</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c2285-b3a1f17314260b0497b436fe03e24655d38e74a76f6caba96f16aa1926a7e9513</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Keles, E</creatorcontrib><creatorcontrib>Kitzmann, D</creatorcontrib><creatorcontrib>Mallonn, M</creatorcontrib><creatorcontrib>Alexoudi, X</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Pino, L</creatorcontrib><creatorcontrib>Seidel, J V</creatorcontrib><creatorcontrib>Carroll, T A</creatorcontrib><creatorcontrib>Steffen, M</creatorcontrib><creatorcontrib>Ilyin, I</creatorcontrib><creatorcontrib>Poppenhäger, K</creatorcontrib><creatorcontrib>Strassmeier, K G</creatorcontrib><creatorcontrib>von Essen, C</creatorcontrib><creatorcontrib>Nascimbeni, V</creatorcontrib><creatorcontrib>Turner, J D</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Keles, E</au><au>Kitzmann, D</au><au>Mallonn, M</au><au>Alexoudi, X</au><au>Fossati, L</au><au>Pino, L</au><au>Seidel, J V</au><au>Carroll, T A</au><au>Steffen, M</au><au>Ilyin, I</au><au>Poppenhäger, K</au><au>Strassmeier, K G</au><au>von Essen, C</au><au>Nascimbeni, V</au><au>Turner, J D</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Probing the atmosphere of HD189733b with the Na i and K i lines</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2020-10-11</date><risdate>2020</risdate><volume>498</volume><issue>1</issue><spage>1023</spage><epage>1033</epage><pages>1023-1033</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
High spectral resolution transmission spectroscopy is a powerful tool to characterize exoplanet atmospheres. Especially for hot Jupiters, this technique is highly relevant, due to their high-altitude absorption, e.g. from resonant sodium (Na i) and potassium (K i) lines. We resolve the atmospheric K i absorption on HD189733b with the aim to compare the resolved K i line and previously obtained high-resolution Na i-D line observations with synthetic transmission spectra. The line profiles suggest atmospheric processes leading to a line broadening of the order of ∼10 km/s for the Na i-D lines and only a few km/s for the K i line. The investigation hints that either the atmosphere of HD189733b lacks a significant amount of K i or the alkali lines probe different atmospheric regions with different temperature, which could explain the differences we see in the resolved absorption lines.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/staa2435</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0003-1231-2194</orcidid><orcidid>https://orcid.org/0000-0002-7990-9596</orcidid><orcidid>https://orcid.org/0000-0001-9770-1214</orcidid><orcidid>https://orcid.org/0000-0003-4269-3311</orcidid><oa>free_for_read</oa></addata></record> |
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| title | Probing the atmosphere of HD189733b with the Na i and K i lines |
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