2013A&A...559A..50N


Query : 2013A&A...559A..50N

2013A&A...559A..50N - Astronomy and Astrophysics, volume 559A, 50-50 (2013/11-1)

Obscuration effects in super-soft-source X-ray spectra.

NESS J.-U., OSBORNE J.P., HENZE M., DOBROTKA A., DRAKE J.J., RIBEIRO V.A.R.M., STARRFIELD S., KUULKERS E., BEHAR E., HERNANZ M., SCHWARZ G., PAGE K.L., BEARDMORE A.P. and BODE M.F.

Abstract (from CDS):

Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ∼3-7x105K and luminosities of 1035–38erg/s. Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. We collected all grating spectra of conventional SSS like Cal83 and Cal87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature. We find two distinct types of SSS spectra that we name SSa and SSe. Their main observational characteristics are either clearly visible absorption lines or emission lines, respectively, while both types contain atmospheric continuum emission. SSa spectra are highly structured with no spectral model currently able to reproduce all details. The emission lines clearly seen in SSe may also be present in SSa, hidden within the forest of complex atmospheric absorption and emission features. This suggests that SSe are in fact obscured SSa systems. Similarities between SSe and SSa with obscured and unobscured AGN, respectively, support this interpretation. We find all known or suspected high-inclination systems to emit permanently in an SSe state. Some sources are found to transition between SSa and SSe states, becoming SSe when fainter. SSS spectra are subject to various occultation processes. In persistent SSS spectra such as Cal87, the accretion disc blocks the central hot source when viewed edge on. In novae during their SSS phase, the accretion disc may have been destroyed during the initial explosion but could have reformed by the time of the SSS phase. In addition, clumpy ejecta may lead to temporary obscuration events. The emission lines stem from reprocessed emission in the accretion disc, its wind or further out in clumpy ejecta, while Thomson scattering allows continuum emission to be visible also during total obscuration of the central hot source.

Abstract Copyright:

Journal keyword(s): novae, cataclysmic variables - X-rays: binaries - binaries: eclipsing

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* QR And CV* 00 19 49.9252996176 +21 56 52.169584416   12.38 12.73 11.86   Ss 128 0
2 V* V723 Cas No* 01 05 05.3607320352 +54 00 40.238720388   15.817 15.484 15.044   ~ 195 0
3 SN 2009A SN* 01 52 44.34 -03 23 48.2           SNIIP 15 1
4 M 77 GiP 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4425 2
5 V* HV Cet CV* 03 05 58.5484640863 +05 47 14.469922873           ~ 35 0
6 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1686 2
7 V* KT Eri No* 04 47 54.2014586736 -10 10 42.962267424   14.986 14.705 15.099   ~ 122 0
8 LMCN 2012-03a No* 04 54 56.8512303744 -70 26 56.406602868           ~ 28 0
9 SV* HV 5682 XB* 05 13 50.7836696744 -69 51 47.483136927     16.566 16.606 16.62 ~ 313 0
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16509 1
11 2E 1550 XB* 05 43 34.1600044704 -68 22 22.191505716   15.9   17.2 16.54 ~ 318 0
12 OGLE LMC-SC20 113500 EB* 05 46 46.54 -71 08 53.9     19.163   18.886 ~ 251 0
13 V* V959 Mon No* 06 39 38.5986803977 +05 53 52.878876073           ~ 145 0
14 V* T Pyx CV* 09 04 41.5061511720 -32 22 47.502932700           ~ 414 0
15 V* V395 Car LXB 09 22 34.6761959832 -63 17 41.355773520 15.40 15.90 15.3     ~ 125 0
16 V* OY Car CV* 10 06 22.0793274312 -70 14 04.584660540           ~ 560 0
17 V* V382 Vel No* 10 44 48.3975221712 -52 25 31.168268472   15.945 15.737 16.173   ~ 184 0
18 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1586 0
19 NAME Upper Sco Association As* 16 12 -23.4           ~ 1252 1
20 V* U Sco CV* 16 22 30.7791646104 -17 52 43.166822628           F8+K2 521 0
21 V* RS Oph Sy* 17 50 13.1591484960 -06 42 28.480729788   11.884 10.776 11.228   K5.5/M0IIIe 1036 0
22 V* V5116 Sgr No* 18 17 50.7277266627 -30 26 32.079704535     19.181   18.962 ~ 62 0
23 V* V4743 Sgr No* 19 01 09.3393890856 -22 00 06.016418064           ~ 138 0
24 V* V1494 Aql No* 19 23 05.3600241442 +04 57 19.811779912           ~ 154 0
25 V* V2491 Cyg CV* 19 43 01.9771342416 +32 19 13.549047276 18.27 18.72 18.03 17.72 17.41 ~ 155 0
26 V* WZ Sge CV* 20 07 36.5037622512 +17 42 14.733254952   15.30 15.20     DAepv 928 0
27 V* SS Cyg CV* 21 42 42.8034497592 +43 35 09.867842484 11.07 12.651 12.032 9.326   K5V 1267 1

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2023.01.31-01:30:36

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