Chandra Observations of the Recurrent Nova IM Normae

  title={Chandra Observations of the Recurrent Nova IM Normae},
  author={Marina Orio and Emre Tepedelenlioglu and Sumner Starrfield and Charles E. Woodward and Massimo Della Valle},
  journal={The Astrophysical Journal},
  pages={938 - 942}
The recurrent nova IM Nor was observed twice in X-rays with the Chandra ACIS-S, 1 and 6 months after the optical outburst. It was not detected in the first observation, with an upper limit on the X-ray luminosity in the 0.2-10 keV range LX < 4.8 × 1030(d kpc-1)2 ergs s-1 (where d is the distance to the nova). Five months later, a hard X-ray source with LX = × 1032(d kpc)2 ergs s-1 was detected. The X-ray spectrum appears to be thermal, but we cannot rule out additional components due to… 

Figures and Tables from this paper

Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)
Observing the X-ray emission from only one day after the nova discovery, the source is followed through the initial brightening, the super-soft source phase and back to the pre-outburst flux level, demonstrating the evolution of the spectrum throughout the outburst.
Novae as a Class of Transient X-Ray Sources
Motivated by the recently discovered class of faint (1034-1035 ergs s−1) X-ray transients in the Galactic center region, we investigate the 2-10 keV properties of classical and recurrent novae.
The XMM-Newton detection of extended emission from the nova remnant of T Pyxidis
We report the detection of an extended X-ray nebulosity with an elongation from north-east to south-west in excess of 15 arcsec in a radial profile and imaging of the recurrent nova T Pyx using the
Swift observations of 52 Galactic/Magellanic Cloud novae are presented indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst and two optical phenomena are confirmed that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency ofX-ray campaigns.
Observations of galactic and extragalactic novae
The recent GAIA DR2 measurements of distances to galactic novae have allowed to re-analyse some properties of nova populations in the Milky Way and in external galaxies on new and more solid
The secrets of T Pyxidis - II. A recurrent nova that will not become a SN Ia
Aims. We compare the observed and theoretical parameters for the quiescent and outburst phases of the recurring nova T Pyx. Methods. IUE data were used to derive the disk luminosity and the mass
I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only
Recurrent Novae: What Do We Know about Them?
  • G. Anupama
  • Physics
    Proceedings of the International Astronomical Union
  • 2011
Abstract Recurrent novae (RNe) belong to the group of cataclysmic variables that exhibit nova outbursts at intervals on the order of decades. They are rare, with 10 Galactic RNe known to date. Two
A new catalogue of Galactic novae: investigation of the MMRD relation and spatial distribution
In this study, a new Galactic novae catalogue is introduced collecting important parameters of these sources such as their light curve parameters, classifications, full width half maximum (FWHM) of


X-ray emission from classical and recurrent-novae observed with ROSAT
We have analysed 350 pointed and serendipitous observations of 108 different classical and recurrent novae in outburst and in quiescence, contained in the ROSAT archive. One aim was to search for
XMM-Newton observations of Nova LMC 2000
We report on three X-ray observations of Nova LMC 2000 with XMM-Newton at 17, 51 and 294 days after the maximum, respectively. X-ray spectral fits show a concordant decrease of the absorbing column
The evolution of Nova V382 Velorum 1999
We report results of spectroscopic observations of V382 Vel (Nova Vel 1999) carried out at La Silla between 5 and 498 days after maximum light (23 May 1999, V(max) 2:3 0:1). The analysis of the
Recurrent nova IM Normae
We detected the second historical outburst of the 1920 nova IM Nor. Accurate astrometry of the outbursting object revealed the true quiescent counterpart having a magnitude of R = 17.0 mag and B =
The Early X-Ray Emission from V382 Velorum (Nova Velorum 1999): An Internal Shock Model
We present the results of ASCA and RXTE observations of the early X-ray emission from the classical nova V382 Velorum. Its ASCA spectrum was hard (kT ~ 10 keV) with strong (1023 cm-2) intrinsic
A Chandra Low Energy Transmission Grating Spectrometer Observation of V4743 Sagittarii: A Supersoft X-Ray Source and a Violently Variable Light Curve
V4743 Sagittarii (Nova Sgr 2002 No. 3) was discovered on 2002 September 20. We obtained a 5 ks ACIS-S spectrum in 2002 November and found that the nova was faint in X-rays. We then obtained a 25 ks
The 2000 outburst of the recurrent nova CI Aquilae: Optical spectroscopy
We present low- and medium resolution spectra of the recurrent nova CI Aquilae taken at 14 epochs in May and June, 2000. The overall appearance is similar to other U Sco-type recurrent novae (U Sco,
Recurrent novae as a consequence of the accretion of solar material onto a 1. 38 M/sub sun/ white dwarf
We have computed three evolutionary sequences which treat the accretion of hydrogen-rich material onto 1.38 M/sub sun/ white dwarfs. In each of these sequences the accreting matter had only a solar
Revised Analysis of the Supersoft X-Ray Phase, Helium Enrichment, and Turnoff Time in the 2000 Outburst of the Recurrent Nova CI Aquilae
Recurrent nova CI Aquilae entered the final decline phase a bit before 2001 May, about 300 days after the optical maximum, showing the slowest evolution among recurrent novae. Based on the optically
Ultraviolet spectroscopy of the recurrent nova U Scorpii during outburst
Observations of the recurrent nova U Sco during the 1979 outburst are presented, and the spectral evolution is found to differ from that of other recurrent novas. Spectra are dominated by emission