Chandra HETG Spectroscopy of the VY Sculptoris Star TT Ari

Details Chandra HETG Spectroscopy of the VY Sculptoris Star TT Ari Chandra HETG Spectroscopy of the VY Sculptoris Star TT Ari

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1657m&link_type=abstract

Chandra Proposal ID #06300176

Physics

Chandra Proposal Id #06300176

Scientific paper

Existing data indicate that high mass-accretion rate (Mdot) nonmagnetic cataclysmic variables (nmCVs) like novalike variables, VY Scl stars, and dwarf novae in outburst have X-ray spectra that are far more interesting (have brighter lines arising from a broader range of ionization stages) than those of low-Mdot nmCVs like dwarf novae in quiescence. However, most of the nmCVs already targeted by Chandra and XMM are dwarf novae in quiescence. We propose to remedy the imbalance between low-Mdot and high-Mdot nmCVs by observing the brightest VY Scl star, TT Ari, with the Chandra HETG. With this spectrum we will constrain the emission measure distribution, line velocity widths, abundances, density, and geometry of the X-ray-emitting plasma, thereby constraining the boundary layer parameters.

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