2005A&A...440.1079R


Query : 2005A&A...440.1079R

2005A&A...440.1079R - Astronomy and Astrophysics, volume 440, 1079-1086 (2005/9-4)

Long-term optical/IR variability of the Be/X-ray binary LS V +44 17/RX J0440.9+4431.

REIG P., NEGUERUELA I., FABREGAT J., CHATO R. and COE M.J.

Abstract (from CDS):

We present the first long-term study of the optical counterpart to the X-ray pulsar RX J0440.9+4431/LS V +44 17. The data consist of optical spectroscopic and infrared photometric observations taken during the period 1995-2005. The infrared observations are the first published for this source. The results of our photometric and spectroscopic analysis show that RX J0440.9+4431/LS V +44 17 contains a moderately reddened, E(B-V)=0.65±0.05, B0.2V star located at about 3.3kpc. The Hα line consistently shows a double-peak profile varying from symmetric shape to completely distorted on one side (V/R phases). A correlation between the equivalent width of the Hα line and the infrared magnitudes is seen: as the EW(Hα) decreases the IR magnitudes become fainter. This long-term optical/IR variability is attributed to structural changes in the Be star's circumstellar disc. The observations include a recent decline in the circumstellar disc and subsequent recovery. We have witnessed the cessation of a global oscillation due to the decline of the circumstellar disc. If the present disc growth rate continues we predict the onset of another episode of V/R variability by the end of 2006. We have investigated the typical time scales for disc variability of various Be/X-ray binaries and found a correlation with the orbital period. This correlation is hard to establish due to the difficulty in defining the exact duration of the various activity states, but it is seen both in the duration of the disc growth/dissipation phase and the value of the Hα equivalent width prior to the appearance of asymmetric profiles. These relationships provide further evidence for the interaction of the neutron star with the circumstellar disc of the Be star's companion and confirms the need of a fully developed disc for the V/R variability to be observed.

Abstract Copyright:

Journal keyword(s): stars: individual: RX J0440.9+4431, LS V +44 17 - X-rays: binaries - stars: neutron - stars: binaries: close - stars: emission-line, Be

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* V635 Cas HXB 01 18 31.9704955824 +63 44 33.072603144 17.05 16.64 15.19 14.34 13.22 B0.2Ve 695 0
2 EM* GGA 104 HXB 01 47 00.2124077208 +61 21 23.663788056 11.76 12.09 11.366 11.00 10.52 B1IIIe 177 0
3 V* BQ Cam HXB 03 34 59.9116110096 +53 10 23.296879776   17.16 15.42 14.26 13.04 O8.5Ve 435 1
4 V* X Per HXB 03 55 23.0777456088 +31 02 45.039836148 6.090 6.840 6.720     O9.5III 940 0
5 LS V +44 17 HXB 04 40 59.3296237272 +44 31 49.258049376 11.02 11.42 10.73 10.28 9.76 B0.2Ve 106 0
6 HD 245770 HXB 05 38 54.5748918624 +26 18 56.836952784 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 931 0
7 V* V572 Pup HXB 08 12 28.3575205680 -31 14 52.138451400 12.14 13.03 12.74 12.44   B0.2IVe 63 0
8 HD 102567 Be* 11 48 00.0214464120 -62 12 24.902384760 8.24 9.06 9.00 9.62   O/Bne 300 0
9 GSC 03588-00834 HXB 21 03 35.7100848936 +45 45 05.568751692   15.34 14.20 13.49 12.75 B0Ve 163 0

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2022.10.02-14:28:09

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