Physics – Fluid Dynamics
Scientific paper
Feb 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasp..107..136s&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 107, no. 708, p. 136-144
Physics
Fluid Dynamics
5
Charge Coupled Devices, Eclipsing Binary Stars, Ephemerides, Light Curve, Stellar Models, Stellar Spectrophotometry, Angular Momentum, K Stars, Stellar Evolution, Stellar Magnitude, Stellar Mass, Stellar Winds
Scientific paper
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 approximately 5 x 10-8 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 approximately 20% and a mass ratio of approximately 0.5. A substantial temperature difference of approximately 400 K 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.
Carrigan Brian J.
Gray Jamison D.
Kreidl Tobias J.
Samec Ronald G.
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