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Title:
Monitoring the Mass Accretion Rate in Scorpius X-1 Using the Optical Johnson B Filter
Authors:
McNamara, B. J.; Norwood, J.; Harrison, T. E.; Holtzman, J.; Dukes, R.; Barker, T.
Affiliation:
AA(Astronomy Department, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003; , , , ), AB(Astronomy Department, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003; , , , ), AC(Astronomy Department, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003; , , , ), AD(Astronomy Department, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003; , , , ), AE(Department of Physics and Astronomy, College of Charleston, 101 Science Center, 58 Coming Street, Charleston, SC 29424; ), AF(Department of Physics and Astronomy, Wheaton College, Norton, MA 02766; )
Publication:
The Astrophysical Journal, Volume 623, Issue 2, pp. 1070-1075. (ApJ Homepage)
Publication Date:
04/2005
Origin:
UCP
ApJ Keywords:
Stars: Mass Loss, X-Rays: Binaries, X-Rays: Individual: Constellation Name: Scorpius X-1
DOI:
10.1086/428640
Bibliographic Code:
2005ApJ...623.1070M

Abstract

The emission from low-mass X-ray binaries (LMXBs) arises from the accretion of mass onto a neutron star or black hole. A knowledge of the amount of mass being accreted as well as changes in this value are therefore essential inputs into models of these systems. Despite the need for this information, we currently lack an easily applied method that allows the accretion rate to be measured. X-ray color-color plots and UV observations can be used for this purpose, but these methods require access to oversubscribed satellites. Even if time is granted on these facilities, there is no guarantee that the source will be in a desired state when the observations take place. In this paper we show that an estimate of the ratio of the mass accretion rate to the Eddington rate can be obtained for Sco X-1 by using the Johnson B magnitude. Based on correlated X-ray and ground-based observations, we find that for Sco X-1, M˙/M˙E=-(0.123+/-0.007)B+2.543+/-0.085. This relation is valid when the system is on its normal and lower flaring branches. Based on theoretical models, we suggest that similar relations should also exist for other LMXBs.
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