期刊
ASTROPHYSICAL JOURNAL
卷 754, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/754/1/20
关键词
accretion, accretion disks; pulsars: individual (A 0535+26); stars: emission-line, Be; stars: neutron; X-rays: binaries
资金
- NASA [NNX08AW06G, NNX11AE24G]
- NASA Postdoctoral Program at NASA Marshall Space Flight Center
- NASA [93862, NNX08AW06G, 146600, NNX11AE24G] Funding Source: Federal RePORTER
- Science and Technology Facilities Council [ST/H002391/1, ST/J001465/1, ST/G009465/1, PP/E001149/1] Funding Source: researchfish
- STFC [PP/E001149/1, ST/J001465/1, ST/G009465/1, ST/H002391/1] Funding Source: UKRI
We present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A 0535+26 with the Fermi/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data (since similar to 1978) and discussed in terms of the neutron-star-Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray quasi-periodic oscillation was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25 keV. In the long term a strong optical/X-ray correlation was found for this system, however in the medium term the H alpha equivalent width and the V-band brightness showed an anti-correlation after similar to 2002 August. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the H alpha showed a strong emission. In late 2010 and before the 2011 February outburst, rapid V/R variations are observed in the strength of the two peaks of the H alpha line. These had a period of similar to 25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V/R variability beginning similar to 6 months following a giant outburst.
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