Pulsation analysis of V 588 MON AND V 589 MON observed with the MOST AND CoRoT satellites

Show simple item record

dc.creator Zwintz, K.
dc.creator Kallinger, T.
dc.creator Guenther, David B.
dc.creator Gruberbauer, Michael
dc.creator Kuschnig, R.
dc.creator Weiss, W. W.
dc.creator Auvergne, M.
dc.creator Jorda, L.
dc.creator Favata, F.
dc.creator Matthews, J.
dc.creator Fischer, M.
dc.date.accessioned 2013-11-01T15:51:55Z
dc.date.available 2013-11-01T15:51:55Z
dc.date.issued 2011-03-01
dc.identifier.issn 0004-637X
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/25311
dc.description Publisher's version/PDF
dc.description.abstract The two pulsating pre-main sequence (PMS) stars V 588 Mon and V 589 Mon were observed by CoRoT for 23.4 days in 2008 March during the Short Run SRa01 and in 2004 and 2006 by MOST for a total of ∼70 days. We present their photometric variability up to 1000μHz and down to residual amplitude noise levels of 23 and 10 ppm of the CoRoT data for V 588 Mon and V 589 Mon, respectively. The CoRoT imagette data as well as the two MOST data sets allowed for detailed frequency analyses using Period04 and SigSpec.We confirm all previously identified frequencies, improve the known pulsation spectra to a total of 21 frequencies for V 588 Mon and 37 for V 589 Mon, and compare them to our PMS model predictions. No model oscillation spectrum with l = 0, 1, 2, and 3 p-modes matches all the observed frequencies. When rotation is included we find that the rotationally split modes of the slower rotating star, V 589 Mon, are addressable via perturbative methods while for the more rapidly rotating star, V 588 Mon, they are not and, consequently, will require more sophisticated modeling. The high precision of the CoRoT data allowed us to investigate the large density of frequencies found in the region from 0 to 300μHz. The presence of granulation appears to be a more attractive explanation than the excitation of high-degree modes. Granulation was modeled with a superposition of white noise, a sum of Lorentzian-like functions, and a Gaussian. Our analysis clearly illustrates the need for a more sophisticated granulation model. en_CA
dc.language.iso en en_CA
dc.publisher American Astronomical Society en_CA
dc.publisher IOP Publishing
dc.relation.uri http://dx.doi.org/10.1088/0004-637X/729/1/20
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Astroseismology
dc.subject.lcsh Variable stars
dc.subject.lcsh Delta Scuti stars
dc.title Pulsation analysis of V 588 MON AND V 589 MON observed with the MOST AND CoRoT satellites en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal 729(1), 20. (2011)


Files in this item


 

Copyright statement:

 
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: http://dx.doi.org/10.1088/0004-637X/729/1/20
 
 

This item appears in the following Collection(s)

Show simple item record