Probing the accretion disk structure and dust distribution along the LOS of the ``Big Dipper'' 4U 1624-490

Details Probing the accretion disk structure and dust distribution along the LOS of the ``Big Dipper'' 4U 1624-490 Probing the accretion disk structure and dust distribution along the LOS of the ``Big Dipper'' 4U 1624-490

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.213x&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

Computer Science

Accretion And Outflows

Scientific paper

High-resolution spectra of low mass X-ray dipping sources would reveal the strong absorption line structures, which could be used for a better understanding of the accretion disk structure. Here, we present a detailed spectral study and X-ray dust scattering halo results of the ``Big Dipper'' 4U 1624-490, based on our Chandra HETGS observation over the 76 ks binary orbit. While the data indicate a possible quasi-sinusoidal modulation with period of ˜43 ks that might be due to changes in local obscuration, the first observed evolution of the iron absorption lines during persistent phase indicates a two-temperature plasma for their origin: a highly ionized component (T˜3.0 × 10^6 K) associated with an extended accretion disk corona of radius R˜3 × 10^10 cm and a less ionized more variable component (T˜1.0 × 10^6 K) coincident with the accretion disk rim. We also estimate a geometric distance to the source to be ˜15 kpc, based on the analysis of halo light curve. Through the analysis of halo radial profiles, we also determine the location, uniformity, and density of ISM dust grains. Our studies of the 4U 1624-490 X-ray halo suggest that a large fraction of the column is local to the X-ray binary. Based on these studies, a viewing geometry that is mapped to changes in plasma conditions over the 4U 1624-490 orbital period is constructed.

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