The CHANDRA data of the classical nova RR Pic (1925): A possible magnetic cataclysmic variable candidate

Date

2002-12-13

Author

Balman, Şölen
Kupcu-Yoldas, A

Metadata

Show full item record

This work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

Item Usage Stats

85
views

0
downloads

During 25ksec of CHANDRA ACIS-S3 observations of the old nova RR Pic 1925 a count rate of 0.067 +/- 0.0017 c/s was detected. The results show evidence (spatial and spectral) for X-ray emission from the region around the prominent SW blob in the Ha images. Shell emission is detected with count rate greater than or equal to (1.95 +/- 1.33)X10(-3) c/s. The spectral analysis shows that the source spectrum can not be explained by a single or two temperature bremsstrahlung or VMEKAL models including photoelectric absorption, only models using powerlaw distribution of temperature fit the data well and indicate excess O, Al, Mg, S, and Si in the source spectrum. A soft excess in the CHANDRA data could be explained by a partial covering absorber model with covering fraction in a range 14-86% consistent with characteristics of the Magnetic Cataclysmic Variable systems. The light curve shows significant orbital and other modulations.

Subject Keywords

Remnants

URI

https://hdl.handle.net/11511/53556

Collections

Department of Physics, Conference / Seminar

Suggestions

OpenMETU
Core

The effect of double austenitization on the microstructure and toughness of AISI M2 high speed steel Ögel, Bilgehan (1998-06-01) In this study, the effect of double austenitization on microstructure and toughness of AISI M2 high speed steel was investigated. For double austenitization treatment, the specimens, which are hardened initially at 1220 degrees C and quenched in air, were hardened for a second time in the temperature range 1150 - 1050 degrees C. For comparison purposes, another set of specimens is austenitized singly in the temperature range 1150 - 1050 degrees C. Tempering process was carried out between 500 - 640 degrees ...
The CHANDRA observation of the first resolved and detected classical nova shell in X-rays: The shell of Nova Persei 1901 (GK Per) Balman, Şölen (2000-09-09) I present the CHANDRA ACIS-S data of the classical nova shell of Nova Persei (1901). The X-ray nebula is detected with a count rate of 0.10+/-0.003 c s(-1). It is asymmetric with bulk of emission on the southwestern quadrant. The X-ray emission from the vicinity of the radio ridge is detected as an arc that covers from west to south of the central source. The X-ray spectrum consists at least of two components of emission. The lower temperature component (below 2 keV) has kT 0.15+/-0.02 keV with an X-ray flu...
The first resolved and detected classical nova shell in X-rays: The shell of Nova Persei 1901 Balman, Şölen; Ogelman, HB (IOP Publishing, 1999-06-20) We present the ROSAT High-Resolution Imager data of the first resolved and detected classical nova shell in the X-ray wavelengths: the shell of Nova Persei 1901. We find that the X-ray nebula is composed of knots/clumps and has an elliptical shape with a total count rate of about 0.01 +/- 0.001 counts s(-1). We estimate that the spectrum is of thermal origin with a luminosity of similar to 8.0 x 10(31) ergs s(-1) and an X-ray temperature of similar to 2.0 x 10(6) K in the 0.1-2.4 keV energy range. The knots...
The X-ray spectral evolution of classical Nova V1974 Cygni 1992: A reanalysis of the ROSAT data Balman, Şölen; Krautter, J; Ogelman, H (IOP Publishing, 1998-05-20) We present a spectral analysis of the archival X-ray data of classical Nova V1974 Cygni 1992 (Nova Cygni 1992) obtained by the ROSAT Position Sensitive Proportional Counter (PSPC). The X-ray spectrum is fitted with a two-component model. The first component is a white dwarf atmosphere emission model developed for the remnants of classical novae near the Eddington luminosity. The model is used to fit the soft X-ray data in the similar to 0.1-1.0 keV range, where the bulk of emission is below 0.7 keV. The sec...
Analysis of chandra data of the old classical nova rr pic (1925) Pekön, Yakup; Balman, Şölen; Department of Physics (2007) In this work, the CHANDRA ACIS-S3 data of the old classical nova RR Pic (1925) is presented. The source is detected with a count rate of 0.067 (+-0.002) c/s in the 0.3-5.0 keV energy range. The orbital period of the binary system in X-ray wavelengths is detected. X-ray spectrum of RR Pic can be represented by a composite model of bremsstrahlung with a photoelectric absorption, two absorption lines centered around 1.1-1.4 keV and 5 Gaussian emission lines centered at around 0.3-1.1 keV . The best t bremsstra...

Citation Formats

Ş. Balman and A. Kupcu-Yoldas, “The CHANDRA data of the classical nova RR Pic (1925): A possible magnetic cataclysmic variable candidate,” 2002, vol. 315, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/53556.