2018ApJ...858...78G


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.21CET10:36:03

2018ApJ...858...78G - Astrophys. J., 858, 78-78 (2018/May-2)

The temporal development of dust formation and destruction in nova Sagittarii 2015#2 (V5668 SGR): a panchromatic study.

GEHRZ R.D., EVANS A., WOODWARD C.E., HELTON L.A., BANERJEE D.P.K., SRIVASTAVA M.K., ASHOK N.M., JOSHI V., EYRES S.P.S., KRAUTTER J., KUIN N.P.M., PAGE K.L., OSBORNE J.P., SCHWARZ G.J., SHENOY D.P., SHORE S.N., STARRFIELD S.G. and WAGNER R.M.

Abstract (from CDS):

We present 5-28 µm SOFIA FORECAST spectroscopy complemented by panchromatic X-ray through infrared observations of the CO nova V5668 Sgr documenting the formation and destruction of dust during ∼500 days following outburst. Dust condensation commenced by 82 days after outburst at a temperature of ∼1090 K. The condensation temperature indicates that the condensate was amorphous carbon. There was a gradual decrease of the grain size and dust mass during the recovery phase. Absolute parameter values given here are for an assumed distance of 1.2 kpc. We conclude that the maximum mass of dust produced was 1.2 x 10–7 M if the dust was amorphous carbon. The average grain radius grew to a maximum of ∼2.9 µm at a temperature of ∼720 K around day 113 when the shell visual optical depth was τv ∼ 5.4. Maximum grain growth was followed by a period of grain destruction. X-rays were detected with Swift from day 95 to beyond day 500. The Swift X-ray count rate due to the hot white dwarf peaked around day 220, when its spectrum was that of a kT = 35 eV blackbody. The temperature, together with the supersoft X-ray turn-on and turn-off times, suggests a white dwarf mass of ∼1.1 M. We show that the X-ray fluence was sufficient to destroy the dust. Our data show that the post-dust event X-ray brightening is not due to dust destruction, which certainly occurred, as the dust is optically thin to X-rays.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): circumstellar matter - infrared: stars - novae, cataclysmic variables - stars: individual: V5668 Sgr - stars: winds, outflows

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 Hilt 102 * 01 09 05.0413010293 +62 47 30.265788867 10.88 11.10 10.42     B0III 44 0
2 NOVA Eri 2009 No* 04 47 54.21 -10 10 43.1           ~ 104 0
3 BD+52 913 WD* 05 05 30.6182785658 +52 49 51.920797126 10.25 11.44 11.69 11.93 12.108 DA.8 970 0
4 NOVA Mon 2012 No* 06 39 38.74 +05 53 52.0           ~ 115 0
5 BD+33 2642 pA* 15 51 59.8857490337 +32 56 54.327647794 9.806 10.61 10.73 10.884 10.961 O7p 370 0
6 V* RS Oph No* 17 50 13.1592776879 -06 42 28.481553668   12.29 4.30     OB+M2ep 918 0
7 NOVA Ser 1978 No* 17 51 50.89 -14 43 50.6           ~ 75 0
8 HD 168646 * 18 22 00.1409435214 -28 25 47.880634994   6.396 6.154     A3III 27 0
9 V* V5568 Sgr Al* 18 25 24.6443312637 -22 11 16.444893279       13.46   ~ 7 0
10 NOVA Sgr 2015 b No* 18 36 57.00 -28 55 42.0           ~ 66 0
11 * phi Sgr PM* 18 45 39.3861043 -26 59 26.794441 2.69 3.050 3.140     B8III 109 0
12 V* NQ Vul No* 19 29 14.751 +20 27 59.63   7.5       ~ 150 0
13 HD 338808 HS* 19 44 26.1388988534 +26 13 16.682298603 10.92 11.03 10.47     sdB0.5VIpHe9 88 0
14 NOVA Del 2013 No* 20 23 30.6864752010 +20 46 03.777415270   17.50 16.86     ~ 154 0
15 V* V1974 Cyg No* 20 30 31.61 +52 37 51.3           ~ 533 0
16 NOVA Cyg 2006 No* 21 11 32.346 +44 48 03.66   10.5 8.5     ~ 90 1
17 NOVA Cyg 1978 No* 21 42 35.22 +44 01 54.9   20.0       ~ 213 0
18 V* V705 Cas No* 23 41 47.19 +57 30 59.5           ~ 178 0

    Equat.    Gal    SGal    Ecl

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2020.02.21-10:36:03

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