Difference between revisions of "A0535+26"
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(Created page with "Category:Accreting X-ray Pulsars '''This page is still edited''' = System Overview = {| class="wikitable" |P<sub>orb</sub> | 111.1 | days | Finger et al. 2006 |-...") |
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Latest revision as of 14:20, 18 April 2018
This page is still edited
System Overview
Porb | 111.1 | days | Finger et al. 2006 |
Pspin | 103.4 | s | Rosenberg et al. 1975, Makino et al. 1989, ... |
B | 4x1012 | G | Kendziorra et al. 1994 |
a sin i | 267 | lt-sec | Finger et al. 2006 |
eccentricity | 0.47 | Finger et al. 2006 | |
ω | 130 | degree | Finger et al. 2006 |
Τperiastron | 53613.0 | MJD | Finger et al. 2006 |
distance | 2 | kpc | Steele et al. 1994 |
Optical companion
HDE 245770, spectral class: O9.7IIIe (Giangrande et al. 1980), B0 IIIe (Steele et al. 1998)
M | 14 / 20 / 26 | M⊙ | de Loore et al. 1984 / Coe et al. 2006 / Haigh et al. 2004 |
R | 14 | R⊙ | de Loore et al. 1984 |
Mdot | 10-8 | M⊙ | de Loore et al. 1984 |
Teff | 26000-28000 | K | Giovannelli & Graziati 1992 |
L | 0.7 x 105 | L⊙ | Giovannelli & Graziati 1992 |
Description
Pulse period and pulse profiles
- pulse shape and intensity are highly variable (Frontera et al. 1985)
- lower energies several, irregularly spaced maxima observed (bradt et al. 1976)
- double-peaked pulse profiles above 20 keV
- asymmetric main and more symmetric secondary peak (Kendziorra et al. 1994)
- pulsed fraction increases with energy (Frontera et al. 1985, Kendziorra et al. 1994)
Spectrum
- hard power law with index 0.8-1.1 with exponential cutoff (Ricketts et al. 1975, Kendziorra et al. 1994)
- 2 cyclotron lines at about 50, 100 keV
- Pulse phase analysis: main pulse spectrum harder than secondary pulse (Kendziorra et al. 1994)