Find rare variable sources

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Goal 4: To find rare variable sources

The massive variability dataset and multicolour atlas will allow us to search for: CVs (novae, dwarf novae) and other eruptive variables (e.g. RSCVn), eclipsing binary RR Lyrae, pre-HB/post He-flash stars, eclipsing binary clump giants, binary microlensing events, LBVs, FU Ori protostars undergoing unstable accretion, and AGB stars at the stage of unstable shell burning. With the advent of Chandra, XMM, INTEGRAL, and the Cerenkov telescopes, a number of persistent and transient high-energy sources have been discovered towards the inner Milky Way, with their locations pinpointed accurately[1]. We will also be able to identify the counterparts of high energy (X-ray and γ-ray ) sources: accreting black holes, microquasars[2], binary pulsar companions, LMXBs, and HMXBs. In particular, this survey may finally reveal the still undetected counterparts of the most luminous persistent hard X-ray/jet sources in the Galactic Center region, 1E 1740.7-2942[3] and GRS 1758-258[4]. A caveat is that although we would identify and monitor the counterparts of several variable high-energy sources, we do not claim to be able to determine orbital periods for all XRB counterparts given the sampling. However, the possibility of other time-variable serendipitous discoveries is open.

References

  1. Aharonian et al. 2006, A&A, in press; Kuulkers et al. 2006, astro-ph/0603130
  2. e.g. Mirabel & Rodriguez 1998, Nature, 392, 673
  3. Mirabel et al. 1992, Nature 358, 215
  4. Rodriguez, Mirabel & Marti 1992, ApJ 405, L15
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