Afficher la notice abrégée

Exoplanet Magnetic Field Estimation via Energetic Neutral Atoms (ENAs) and Hydrogen Cloud Observations and Modelling

dc.contributor.authorLAMMER, H.
dc.contributor.authorKISLYAKOVA, K. G.
hal.structure.identifierSwedish Institute of Space Physics [Uppsala / Kiruna] [IRF]
dc.contributor.authorHOLMSTRÖM, M.
dc.contributor.authorKHODACHENKO, M. L.
dc.contributor.authorGRIESSMEIER, Jean-Mathias
hal.structure.identifierPhysikalisches Institut [Bern]
dc.contributor.authorWURZ, P.
hal.structure.identifiersSE 2011
dc.contributor.authorSELSIS, Franck
dc.contributor.authorHANSLMEIER, A.
dc.date.issued2011
dc.date.conference2010
dc.description.abstractEnThe discovery of more than 500 exoplanets during the past 15 years has enabled us to characterize the upper atmosphere structure of some exosolar gas giants and to compare observational and modelling results to the known planets in the Solar System. It is of great interest to understand if these exosolar "Hot Jupiters" share similar physical processes compared to the giant planets (Jupiter and Saturn) in the Solar System with regard to their magnetic dynamos and the corresponding expected magnetic field strengths. In this work we discuss how observations of stellar Lyman-alpha absorption by so-called Energetic Neutral Atoms (ENAs) around transiting exoplanets together with theoretical modelling efforts can be used as a tool for estimating magnetic obstacle sizes and the corresponding magnetic field strength. For demonstrating this method we model the production of stellar wind related planetary hydrogen and ENA populations around the exosolar gas giant HD 209458b and show how a detailed analysis of attenuation spectra obtained during transits can be used for the estimation of the planet's magnetic obstacle size and hence its dynamo field strength. Our study indicates that the magnetic field strength of HD 209458b which is able to balance the stellar wind plasma flow by a magnetic obstacle around the planet which can explain the observed Lyman-alpha line profiles observed before and during the transits by HST corresponds to a magnetic dipole moment which is about 40 percent of Jupiters value.
dc.language.isoen
dc.source.titleProceedings of the 7th International Workshop on Planetary, Solar and Heliospheric Radio Emissions (PRE VII), held at Graz, Austria, September 15-17, 2010, p. 303-312
dc.subjectradio emissions
dc.subjectexoplanet
dc.subjectmagnetic field estimation
dc.subjectenergetic neutral atoms
dc.subjecthydrogen cloud onservations
dc.subjectmodelling
dc.title.enExoplanet Magnetic Field Estimation via Energetic Neutral Atoms (ENAs) and Hydrogen Cloud Observations and Modelling
dc.typeCommunication dans un congrès
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
bordeaux.page303-312
bordeaux.conference.title7th International Workshop on Planetary, Solar and Heliospheric Radio Emissions (PRE VII)
bordeaux.countryAT
bordeaux.title.proceedingProceedings of the 7th International Workshop on Planetary, Solar and Heliospheric Radio Emissions (PRE VII), held at Graz, Austria, September 15-17, 2010, p. 303-312
bordeaux.conference.cityGraz
bordeaux.peerReviewedoui
hal.identifierhal-00686386
hal.version1
hal.invitednon
hal.proceedingsoui
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00686386v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.btitle=Proceedings%20of%20the%207th%20International%20Workshop%20on%20Planetary,%20Solar%20and%20Heliospheric%20Radio%20Emissions%20(PRE%20VII),%20held%20at%20Graz,%20Austria,%&rft.date=2011&rft.spage=303-312&rft.epage=303-312&rft.au=LAMMER,%20H.&KISLYAKOVA,%20K.%20G.&HOLMSTR%C3%96M,%20M.&KHODACHENKO,%20M.%20L.&GRIESSMEIER,%20Jean-Mathias&rft.genre=unknown


Fichier(s) constituant ce document

FichiersTailleFormatVue

Il n'y a pas de fichiers associés à ce document.

Ce document figure dans la(les) collection(s) suivante(s)

Afficher la notice abrégée