Query : 2014A&A...562A..28D

2014A&A...562A..28D - Astronomy and Astrophysics, volume 562A, 28-28 (2014/2-1)

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. III. The ultraviolet development from iron curtain through the post-X-ray turnoff.


Abstract (from CDS):

We continue the analysis of the multiwavelength evolution of the recurrent nova T Pyx during its 2011 outburst, focussing on the spectral development on the 1150-3000Å region. This extraordinary data set presents the longest temporal baseline high resolution view of the ultraviolet for any nova to date (classical or recurrent). The observations cover the early Fe-curtain stage, when the UV was completely optically thick, to 834 days after discovery when the outburst was effectively over. We present an analysis of dynamics and abundances of the interstellar species whose resonance lines are accessible in the UV. The Lyα profile is consistent with only interstellar absorption at all epochs and agrees with the HI 21cm column density. The distance obtained to T Pyx is about 5kpc, based on the ISM analysis. For the ejecta evolution we have been able to follow the changes in ionization and structure with previously unobtained resolution and cadence. The excited state isoelectronic transitions of C III, N IV], and O V displayed the same detached absorption lines as the optical He I transitions during the optical maximum. This is explained as resonance absorption within the ejecta of FUV ground state lines from the 300-1000Å range. The resonance lines of all species showed absorption components between -1000 and -3000km/s as soon as the Fe-curtain turned transparent (from day 105); these persisted at the same velocities and varied in strength from one ion to another through day 834. The last ultraviolet spectrum, taken more than 800 days after outburst, showed the same absorption lines on N V and C IV as day 105. There was no evidence of circumstellar absorbers. This and the related observations of profile evolution effectively rule out any wind model for the spectrum. The picture that emerges is of ejecta that became optically thin after visual maximum as the X-ray emission became visible following an outwardly propagating ionization front and for which the ionization stages froze because of ejecta expansion after the end of the soft X-ray illumination.

Abstract Copyright:

Journal keyword(s): novae, cataclysmic variables - line: profiles - stars: individual: T Pyx - ultraviolet: stars - circumstellar matter

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 OGLE 2016-NOVA-1 No* 05 09 58.3903831759 -71 39 52.714123608   16.0   17.0 17.38 ~ 74 0
2 LMCN 1990-01a No* 05 23 21.79 -69 29 48.4           ~ 60 0
3 LMCN 2000-07a No* 05 25 01.63 -70 14 17.4           ~ 23 0
4 V* V959 Mon No* 06 39 38.5986803977 +05 53 52.878876073           ~ 149 0
5 V* T Pyx CV* 09 04 41.5061511720 -32 22 47.502932700           ~ 420 0
6 V* V382 Vel No* 10 44 48.3975221712 -52 25 31.168268472   15.945 15.737 16.173   ~ 188 0
7 V* RS Oph Sy* 17 50 13.1591484960 -06 42 28.480729788   11.884 10.776 11.228   K5.5/M0IIIe 1054 0
8 V* V1974 Cyg No* 20 30 31.6546001712 +52 37 50.837478240           ~ 569 0

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