Observations of 4U 1700-37 with BATSE

被引:41
作者
Rubin, BC
Finger, MH
Harmon, BA
Paciesas, WS
Fishman, GJ
Wilson, RB
Wilson, CA
Brock, MN
Briggs, MS
Pendleton, GN
Cominsky, LR
Roberts, MS
机构
[1] NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,CGRO SCI SUPPORT CTR,HUNTSVILLE,AL 35812
[2] UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899
[3] SONOMA STATE UNIV,DEPT PHYS & ASTRON,ROHNERT PK,CA 94928
关键词
headings; binaries; eclipsing; stars; individual; (4U; 1700-37); neutron; X-rays;
D O I
10.1086/176889
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The eclipsing binary X-ray source 4U 1700-37 has been continually monitored by the BATSE experiment on the Compton Gamma Ray Observatory since the spring of 1991. Using source measurements at times of Earth occultation, we observe an average (uneclipsed) flux of 0.23 crab in the 20-120 keV band. The flux is highly variable, with occasional flaring behavior on timescales from hundreds of seconds to several hours and intensities as bright as 1 crab. The uneclipsed spectrum is well represented by an optically thin thermal bremsstrahlung model with a temperature of 25 keV independent of source intensity or orbital phase. An upper limit of 4% on the pulse fraction has been obtained for pulse periods between 2 and 700 s. Average orbital light curves from almost 1000 days of occultation measurements have been constructed. These profiles are used to measure (1) the eclipse semiangle, theta(E) = 28.degrees 6 +/- 2.degrees 1 in the 20-120 keV band, and (2) the decrease in orbital period, P over dot/P = -(3.3 +/- 0.6) x 10(-6) yr(-1). Estimates of system physical parameters are obtained using Monte Carlo simulations to propagate errors in measured and assumed parameters. For the X-ray source mass we find M(x) = 2.6(-1.4)(+2.3) M., and for the mass and radius of the optical companion, M(0) = 30(-7)(+11) M. and R(0) = 18(-2)(+2) R..
引用
收藏
页码:259 / 270
页数:12
相关论文
共 38 条
[1]   IS GX5-1 A MILLISECOND PULSAR [J].
ALPAR, MA ;
SHAHAM, J .
NATURE, 1985, 316 (6025) :239-241
[2]  
Branduardi G., 1979, Nature, V279, P508, DOI 10.1038/279508a0
[3]   FURTHER COPERNICUS X-RAY OBSERVATIONS OF 3U-1700-37 [J].
BRANDUARDI, G ;
MASON, KO ;
SANFORD, PW .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1978, 185 (01) :137-142
[4]  
BROCK MN, 1992, AIP C P, V280, P709
[5]   WIND-DRIVEN ANGULAR-MOMENTUM LOSS IN BINARY-SYSTEMS .1. BALLISTIC CASE [J].
BROOKSHAW, L ;
TAVANI, M .
ASTROPHYSICAL JOURNAL, 1993, 410 (02) :719-731
[6]   THE ATMOSPHERIC STRUCTURE OF THE O-TYPE SUPERGIANT KRZEMINSKIS STAR AND THE MASS OF ITS COMPANION NEUTRON STAR CENTAURUS X-3 [J].
CLARK, GW ;
MINATO, JR ;
MI, G .
ASTROPHYSICAL JOURNAL, 1988, 324 (02) :974-994
[7]  
CONTI PS, 1978, ASTRON ASTROPHYS, V63, P225
[8]  
CONTI PS, 1975, APJ, V200, P144
[9]   THE HIGH-ENERGY X-RAY-SPECTRUM OF 4U 1700-37 OBSERVED FROM OSO-8 [J].
DOLAN, JF ;
COE, MJ ;
CRANNELL, CJ ;
DENNIS, BR ;
FROST, KJ ;
MAURER, GS ;
ORWIG, LE .
ASTROPHYSICAL JOURNAL, 1980, 238 (01) :238-243
[10]  
DOLAN JF, 1984, ASTRON ASTROPHYS, V139, P249