Chromospheric Models of Solar Type Stars: The Vaughan-Preston Gap

dc.creatorVieytes, Mariela Cristina
dc.creatorMauas, Pablo Jacobo David
dc.date.accessioned2017-08-11T17:58:54Z
dc.date.accessioned2018-11-06T15:59:30Z
dc.date.available2017-08-11T17:58:54Z
dc.date.available2018-11-06T15:59:30Z
dc.date.created2017-08-11T17:58:54Z
dc.date.issued2004-12
dc.identifierVieytes, Mariela Cristina; Mauas, Pablo Jacobo David; Chromospheric Models of Solar Type Stars: The Vaughan-Preston Gap; Springer; Astrophysics And Space Science; 290; 3-4; 12-2004; 311-318
dc.identifier0004-640X
dc.identifierhttp://hdl.handle.net/11336/22202
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1903270
dc.description.abstractWe have built different models for stars of the same spectral type than the Sun but with different levels of chromospheric activity, to study the response of the S index of activity built from the emission of the Ca II H and K lines to changes in the chromospheric structure. We found that the fact that there are many stars with either strong or weak emission, but few with intermediate values of S, the so-called Vaughan Preston gap, can be due to a discontinuity in the response of the Ca II lines to chromospheric heating. In fact, we are able to reproduce the observed distribution of the number of stars as a function of S.
dc.languageeng
dc.publisherSpringer
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1023/B:ASTR.0000032532.94509.5d
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1023/B:ASTR.0000032532.94509.5d
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/restrictedAccess
dc.titleChromospheric Models of Solar Type Stars: The Vaughan-Preston Gap
dc.typeArtículos de revistas
dc.typeArtículos de revistas
dc.typeArtículos de revistas


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