2018A&A...619A.104S


Query : 2018A&A...619A.104S

2018A&A...619A.104S - Astronomy and Astrophysics, volume 619A, 104-104 (2018/11-1)

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta.

SHORE S.N., KUIN N.P., MASON E. and DE GENNARO AQUINO I.

Abstract (from CDS):

A fraction of classical novae form dust during the early stages of their outbursts. The classical CO nova V5668 Sgr (Nova Sgr. 2015b) underwent a deep photometric minimum about 100 days after outburst that was covered across the spectrum. A similar event was observed for an earlier CO nova, V705 Cas (Nova Cas 1993) and a less optically significant event for the more recent CO nova V339 Del (Nova Del 2013). This study provides a "compare and contrast" of these events to better understand the very dynamical event of dust formation. We show the effect of dust formation on multiwavelength high resolution line profiles in the interval 1200Å-9200Å using a biconical ballistic structure that has been applied in our previous studies of the ejecta. We find that both V5668 Sgr and V339 Del can be modeled using a grey opacity for the dust, indicating fairly large grains (≥0.1µ) and that the persistent asymmetries of the line profiles in late time spectra, up to 650 days after the event for V5668 Sgr and 866 days for V339 Del, point to the survival of the dust well into the transparent, nebular stage of the ejecta evolution. This is a general method for assessing the properties of dust forming novae well after the infrared is completely transparent in the ejecta.

Abstract Copyright: © ESO 2018

Journal keyword(s): novae, cataclysmic variables - line: formation - dust, extinction - circumstellar matter

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* V723 Cas No* 01 05 05.3607320352 +54 00 40.238720388   15.817 15.484 15.044   ~ 190 0
2 V* T Aur No* 05 31 59.1180488976 +30 26 45.034081044           ~ 266 0
3 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4722 2
4 V* V959 Mon No* 06 39 38.5986803977 +05 53 52.878876073           ~ 138 0
5 V* T Pyx CV* 09 04 41.5061511720 -32 22 47.502932700           ~ 406 0
6 V* V382 Vel No* 10 44 48.3975221712 -52 25 31.168268472   15.945 15.737 16.173   ~ 179 0
7 V* V1369 Cen No* 13 54 45.3506993424 -59 09 04.093260192   15.5   15.1   ~ 68 0
8 V* U Sco CV* 16 22 30.7791646104 -17 52 43.166822628           F8+K2 513 0
9 V* V1280 Sco No* 16 57 40.91 -32 20 36.4           ~ 95 0
10 V* V1324 Sco No* 17 50 53.9093841216 -32 37 21.090962028           ~ 77 0
11 V* DQ Her CV* 18 07 30.2510391864 +45 51 32.564791872   14.605 14.443 14.800   M3+Ve 990 1
12 V* V5568 Sgr EB* 18 25 24.6443378856 -22 11 16.444042728       13.46   ~ 7 0
13 V* V5668 Sgr CV* 18 36 56.827920 -28 55 39.97524       16.028   ~ 93 0
14 V* V838 Her No* 18 46 31.5739435632 +12 14 00.841303824           ~ 281 0
15 V* V1425 Aql No* 19 05 26.67 -01 42 14.0           ~ 81 0
16 V* V339 Del No* 20 23 30.6873337584 +20 46 03.765339912   17.50 16.86     ~ 177 0
17 V* V1974 Cyg No* 20 30 31.6546001712 +52 37 50.837478240           ~ 560 0
18 V* V2362 Cyg CV* 21 11 32.3419758636 +44 48 03.668158208           ~ 98 0
19 V* V809 Cep No* 23 08 04.71 +60 46 52.1           ~ 16 0
20 V* V705 Cas No* 23 41 47.195448 +57 30 59.57532       16.055   ~ 189 0

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2022.08.16-19:20:08

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