Show simple item record

dc.contributor.author	Morales, Juan Carlos
dc.contributor.author	Ribas, Ignasi
dc.contributor.author	Jordi, Carme
dc.contributor.author	Torres, Guillermo
dc.contributor.author	Gallardo, Jose
dc.contributor.author	Guinan, Edward F.
dc.contributor.author	Charbonneau, David
dc.contributor.author	Wolf, Marek
dc.contributor.author	Latham, David W.
dc.contributor.author	Anglada-Escude, Guillem
dc.contributor.author	Bradstreet, David H.
dc.contributor.author	Everett, Mark E.
dc.contributor.author	O'Donovan, Francis T.
dc.contributor.author	Mandushev, Georgi
dc.contributor.author	Mathieu, Robert D.
dc.date.accessioned	2010-08-12T13:42:32Z
dc.date.issued	2009
dc.identifier.citation	Morales, Juan Carlos, Ignasi Ribas, Carme Jordi, Guillermo Torres, Jose Gallardo, Edward F. Guinan, David Charbonneau, et al. 2009. Absolute properties of the low-mass eclipsing binary CM Draconis. Astrophysical Journal 691(2): 1400-1411.	en_US
dc.identifier.issn	0004-637X	en_US
dc.identifier.issn	1538-4357	en_US
dc.identifier.uri	http://nrs.harvard.edu/urn-3:HUL.InstRepos:4341698
dc.description.abstract	Spectroscopic and eclipsing binary systems offer the best means for determining accurate physical properties of stars, including their masses and radii. The data available for low-mass stars have yielded firm evidence that stellar structure models predict smaller radii and higher effective temperatures than observed, but the number of systems with detailed analyses is still small. In this paper, we present a complete reanalysis of one of such eclipsing systems, CM Dra, composed of two dM4.5 stars. New and existing light curves as well as a radial velocity curve are modeled to measure the physical properties of both components. The masses and radii determined for the components of CM Dra are M 1 = 0.2310 ± 0.0009 M sun, M 2 = 0.2141 ± 0.0010M sun, R 1 = 0.2534 ± 0.0019 R sun, and R 2 = 0.2396 ± 0.0015 R sun. With relative uncertainties well below the 1% level, these values constitute the most accurate properties to date for fully convective stars. This makes CM Dra a valuable benchmark for testing theoretical models. In comparing our measurements with theory, we confirm the discrepancies previously reported for other low-mass eclipsing binaries. These discrepancies seem likely to be due to the effects of magnetic activity. We find that the orbit of this system is slightly eccentric, and we have made use of eclipse timings spanning three decades to infer the apsidal motion and other related properties.	en_US
dc.description.sponsorship	Astronomy	en_US
dc.language.iso	en_US	en_US
dc.publisher	Institute of Physics	en_US
dc.relation.isversionof	doi:10.1088/0004-637X/691/2/1400	en_US
dash.license	OAP
dc.subject	binaries: eclipsing	en_US
dc.subject	binaries: spectroscopic	en_US
dc.subject	stars: late-type	en_US
dc.subject	stars: fundamental parameters	en_US
dc.subject	stars: individual (CM Dra)	en_US
dc.title	Absolute Properties of the Low-Mass Eclipsing Binary CM Draconis	en_US
dc.type	Journal Article	en_US
dc.description.version	Accepted Manuscript	en_US
dc.relation.journal	Astrophysical Journal	en_US
dash.depositing.author	Charbonneau, David
dc.date.available	2010-08-12T13:42:32Z

Files in this item

This item appears in the following Collection(s)

• FAS Scholarly Articles [5137]
  Peer reviewed scholarly articles from the Faculty of Arts and Sciences of Harvard University

Show simple item record

Contact administrator regarding this item (to report mistakes or request changes)