2006/03/31 by A. W. Shafter, K. A. Misselt · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #astro-ph
paper · pdf · doi:10.1086/503764
published as Astrophys.J.644:1104-1117,2006; Erratum-ibid.653:1586,2006 · Accepted for publication in The Astrophysical Journal. Thirty-nine pages, including 9 figures. V2 - updated to include additional references and related discussion to previous work overlooked in the original version, and to correct a typo in the ephemeris given in the abstract. V3 - Minor typos corrected. The paper is scheduled for the 20 June 2006 issue of the ApJ. V4 - An error in equation (9) has been corrected. The results presented in the paper were not affected, as all computations were made using the correct formulation of this equation
openalex publication_date 2006/06/19 · arxiv created 2006/08/03 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
Multicolor ( BVRI ) light curves of the eclipsing classical nova V Per are presented, and a total of 12 new eclipse timings are measured for the system. When combined with previous eclipse timings from the literature, these timings yield a revised ephemeris for the times of mideclipse given by HJD = 2,447,442.8260(1) + 0.107123474(3) E . The eclipse profiles are analyzed with a parameter-fitting model that assumes four sources of luminosity: a white dwarf primary star, a main-sequence secondary star, a flared accretion disk with a rim, and a bright spot at the intersection of the mass transfer stream and the disk periphery. Model parameters include the temperatures of the white dwarf ( T 1 ) and the secondary star ( T 2 ), the radius ( R d ) and temperature ( T d ), of the disk periphery, the inner disk radius ( R in ), the disk power-law temperature exponent (α) and thickness ( h r ), and a bright spot temperature enhancement factor (χ s ). A matrix of model solutions are computed, covering an extensive range of plausible parameter values. The solution matrix is then explored to determine the optimum values for the fitting parameters and their associated errors. For models that treat the accretion disk as a flat structure without a rim, optimum fits require that the disk have a flat temperature profile. Although models with a truncated inner disk ( R in ≫ R 1 ) result in a steeper temperature profile, steady state models with a temperature profile characterized by T ( r ) ∝ r -3/4 are found only for models with a significant disk rim. A comparison of the observed brightness and color at mideclipse with the photometric properties of the best-fitting model suggests that V Per lies at a distance of ~1 kpc.