Analysis of CCD Photometry for the Very Short Period Eclipsing Binary BM Ursae Majoris
CCD images of the fourteenth-magnitude variable BM Ursae Majoris were taken in the spring of 1991 at Lowell Observatory. An RCA CCD camera system and a standard PMT were used. Four times of minimum light were determined and improved linear and quadratic ephemerides were calculated. A period study, s...
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| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 1995-02, Vol.107 (708), p.136-144 |
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| creator | Samec, Ronald G. Gray, Jamison D. Carrigan, Brian J. Kreidl, Tobias J. |
| description | CCD images of the fourteenth-magnitude variable BM Ursae Majoris were taken in the spring of 1991 at Lowell Observatory. An RCA CCD camera system and a standard PMT were used. Four times of minimum light were determined and improved linear and quadratic ephemerides were calculated. A period study, spanning over a thirty-year interval, shows that the system is undergoing a small but continuous period decrease of ~ 5×10⁻ɸ d/yr. This may be due to angular momentum loss (AML) caused by stellar winds. The VRI light curves formed from the present precision observations, show that BM UMa is a W-type W UMa system. The first synthetic light curve solution of BM UMa is also presented. This solution reveals that BM UMa is a contact binary consisting of two early-K spectral-type components with a fill out of ~20% and a mass ratio of ~0.5. A substantial temperature difference of ~400 was determined. Both unspotted and spotted models were calculated. The spotted model indicates the presence of a region of enhanced brightness in the neck of the secondary component. This may be attributed to fluid dynamics of mass in transit rather than to magnetic activity. |
| doi_str_mv | 10.1086/133529 |
| format | Article |
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An RCA CCD camera system and a standard PMT were used. Four times of minimum light were determined and improved linear and quadratic ephemerides were calculated. A period study, spanning over a thirty-year interval, shows that the system is undergoing a small but continuous period decrease of ~ 5×10⁻ɸ d/yr. This may be due to angular momentum loss (AML) caused by stellar winds. The VRI light curves formed from the present precision observations, show that BM UMa is a W-type W UMa system. The first synthetic light curve solution of BM UMa is also presented. This solution reveals that BM UMa is a contact binary consisting of two early-K spectral-type components with a fill out of ~20% and a mass ratio of ~0.5. A substantial temperature difference of ~400 was determined. Both unspotted and spotted models were calculated. The spotted model indicates the presence of a region of enhanced brightness in the neck of the secondary component. 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This may be attributed to fluid dynamics of mass in transit rather than to magnetic activity.</description><subject>Astronomical magnitude</subject><subject>Astronomical photometry</subject><subject>Astronomical research</subject><subject>Ephemerides</subject><subject>Light curves</subject><subject>Mathematical minima</subject><subject>Observational research</subject><subject>Observatories</subject><subject>Stars</subject><subject>Variable stars</subject><issn>0004-6280</issn><issn>1538-3873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1995</creationdate><recordtype>article</recordtype><recordid>eNpFkE9LAzEUxIMoWKt-AyEnb6svefv32K6tCi0WtL0u2fTFpmw3Ndke-u1dqehpGObHMAxjtwIeBOTpo0BMZHHGBiLBPMI8w3M2AIA4SmUOl-wqhC2AELmAAVuNWtUcgw3cGV6WT3yxcZ3bUeeP3DjPuw3xFfXmfeN8xxfkrVvziW7sPtj2k49tq_p0POdLHxTxudo6b8M1uzCqCXTzq0O2nE4-ypdo9vb8Wo5mkZaQdpEWppaISoo0X-s6wxqKrNe1LmqSJiOTUiZqjRDLmjQJiQoVFUZSkWCNOGT3p969d18HCl21s0FT06iW3CFUMotTkBL-Qe1dCJ5Mtfd210-vBFQ_t1Wn23rw7gRuQ-f8HxVDmkMCBX4DabVoMg</recordid><startdate>19950201</startdate><enddate>19950201</enddate><creator>Samec, Ronald G.</creator><creator>Gray, Jamison D.</creator><creator>Carrigan, Brian J.</creator><creator>Kreidl, Tobias J.</creator><general>American Institute of Physics</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>19950201</creationdate><title>Analysis of CCD Photometry for the Very Short Period Eclipsing Binary BM Ursae Majoris</title><author>Samec, Ronald G. ; Gray, Jamison D. ; Carrigan, Brian J. ; Kreidl, Tobias J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c206t-c1fb233a2168dcb73b097cb7dc9be2f7ef6e71bc3042bece123a3ae9f2e953b33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1995</creationdate><topic>Astronomical magnitude</topic><topic>Astronomical photometry</topic><topic>Astronomical research</topic><topic>Ephemerides</topic><topic>Light curves</topic><topic>Mathematical minima</topic><topic>Observational research</topic><topic>Observatories</topic><topic>Stars</topic><topic>Variable stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Samec, Ronald G.</creatorcontrib><creatorcontrib>Gray, Jamison D.</creatorcontrib><creatorcontrib>Carrigan, Brian J.</creatorcontrib><creatorcontrib>Kreidl, Tobias J.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Publications of the Astronomical Society of the Pacific</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Samec, Ronald G.</au><au>Gray, Jamison D.</au><au>Carrigan, Brian J.</au><au>Kreidl, Tobias J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Analysis of CCD Photometry for the Very Short Period Eclipsing Binary BM Ursae Majoris</atitle><jtitle>Publications of the Astronomical Society of the Pacific</jtitle><date>1995-02-01</date><risdate>1995</risdate><volume>107</volume><issue>708</issue><spage>136</spage><epage>144</epage><pages>136-144</pages><issn>0004-6280</issn><eissn>1538-3873</eissn><abstract>CCD images of the fourteenth-magnitude variable BM Ursae Majoris were taken in the spring of 1991 at Lowell Observatory. An RCA CCD camera system and a standard PMT were used. Four times of minimum light were determined and improved linear and quadratic ephemerides were calculated. A period study, spanning over a thirty-year interval, shows that the system is undergoing a small but continuous period decrease of ~ 5×10⁻ɸ d/yr. This may be due to angular momentum loss (AML) caused by stellar winds. The VRI light curves formed from the present precision observations, show that BM UMa is a W-type W UMa system. The first synthetic light curve solution of BM UMa is also presented. This solution reveals that BM UMa is a contact binary consisting of two early-K spectral-type components with a fill out of ~20% and a mass ratio of ~0.5. A substantial temperature difference of ~400 was determined. Both unspotted and spotted models were calculated. The spotted model indicates the presence of a region of enhanced brightness in the neck of the secondary component. 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| source | Jstor Complete Legacy; Institute of Physics Journals; EZB-FREE-00999 freely available EZB journals; Institute of Physics (IOP) Journals - HEAL-Link; Alma/SFX Local Collection |
| subjects | Astronomical magnitude Astronomical photometry Astronomical research Ephemerides Light curves Mathematical minima Observational research Observatories Stars Variable stars |
| title | Analysis of CCD Photometry for the Very Short Period Eclipsing Binary BM Ursae Majoris |
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