English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present X-ray observations of the field containing Nova Puppis 1942 (CPPup) and Nova Puppis 1991 (V351 Pup), done with ASCA in 1998, and withXMM-Newton in 2005. The X-ray and UV luminosity of CP Pup seem to have remainedapproximately constant since the last X-ray observations of the 1980'ies, whilethe optical luminosity has decreased. The X-ray properties of this nova areexplained by a high mass white dwarf accreting at low rate, in agreement withthe nova theory given the large amplitude and other characteristics of the 1942outburst.  Assuming a distance of 1600 pc, the X-ray luminosity of CP Pup is L=2.2 x10(33) erg/s in the 0.15-10 keV range covered with EPIC, compatible with amagnetic system. The RGS grating spectrum shows a few prominent emission lines,and it is fitted with a cooling flow with mass accretion rate mdot <= 1.6 x10(-10) msol/year. We detected also the O VII complex at 21.6-21.8 A that doesnot arise in the cooling flow. Most likely this feature originates in a wind orin the nova shell. The RGS and EPIC spectra are fitted only with thermal modelswith a very high shock temperature, T>60 keV, indicating a white dwarf withM>1.1 M(sun). The X-ray flux is modulated with the spectroscopic period of 1.47hours detected in the optical. Since CP Pup is not an eclipsing system, this isbetter understood if magnetic accretion occurs: we discuss this possibility andits implications in detail. V351 Pup (N Pup 1991) was detected with XMM-Newton,but not with ASCA. It is a faint, non-super-soft X-ray source with luminosityL(x) =~ 3 x 10(31) erg/s, a factor of 50 less than measured with ROSAT in 1993.

New X-ray observations of the old nova CP Puppis and of the more recent nova V351 Pup