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The CHANDRA observation of the first resolved and detected classical nova shell in X-rays: The shell of Nova Persei 1901 (GK Per)
Date
2000-09-09
Author
Balman, Şölen
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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 flux of 6.5x10(-13) erg cm(-2) s(-1). There is also a high temperature, kT > 15 keV, embedded, N-H=1.7+/-0.2x10(22) cm(-2), component prominent above 2 keV. The unabsorbed X-ray flux from this component is 1.1x10(-12) erg cm(-2) s(-1). A distinct emission line of Neon [NeIX] is detected with a flux of 1.5x10(-14) erg cm(-2) s(-1). Enhancement in the elemental abundances of Ne and N compared to their solar mass fractions are detected as 6-9 and 3-6 respectively. The X-ray luminosities indicate that the shock is adiabatic and the remnant is most likely in an early phase of evolution.
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https://hdl.handle.net/11511/53533
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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 first resolved and detected classical nova shell in X-rays in comparison with the ROSAT detections of hard X-ray emission from classical nova in outburst
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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...
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Balman, Şölen; Kupcu-Yoldas, A (2002-12-13)
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...
RR Pic (1925): A Chandra X-ray view
Pekoen, Y.; Balman, Şölen (Oxford University Press (OUP), 2008-08-01)
We present the Chandra ACIS-S3 data of the old classical nova RR Pic (1925). The source has a count rate of 0.067 +/- 0.002 count s(-1) in the 0.3 - 5.0 keV energy range. We detect the orbital period of the underlying binary system in the X- ray wavelengths. We also find that the neutral hydrogen column density differs for orbital minimum and orbital maximum spectra with values 0.25(-0.18)(+0.23) x 10(22) and 0.64(-0.14)(+ 0.13) x 10(22) cm(-2) at 3 sigma confidence level. The X- ray spectrum of RR Pic can ...
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Ş. Balman, “The CHANDRA observation of the first resolved and detected classical nova shell in X-rays: The shell of Nova Persei 1901 (GK Per),” 2000, vol. 234, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/53533.
