The CHANDRA observation of the first resolved and detected classical nova shell in X-rays: The shell of Nova Persei 1901 (GK Per)

Balman S.

X-Ray Astronomy 2000 Conference, MONDELLO, Italy, 4 - 09 September 2000, vol.234, pp.269-274 identifier

  • Publication Type: Conference Paper / Full Text
  • Volume: 234
  • City: MONDELLO
  • Country: Italy
  • Page Numbers: pp.269-274


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.