2018A&A...617A.129K


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.04CEST22:16:30

2018A&A...617A.129K - Astronomy and Astrophysics, volume 617A, 129-129 (2018/9-1)

Submillimeter-wave emission of three Galactic red novae: cool molecular outflows produced by stellar mergers.

KAMINSKI T., STEFFEN W., TYLENDA R., YOUNG K.H., PATEL N.A. and MENTEN K.M.

Abstract (from CDS):

Red novae are optical transients erupting at luminosities typically higher than those of classical novae. Their outbursts are believed to be caused by stellar mergers. We present millimeter/submillimeter-wave observations with the Atacama Large (sub)Millimeter Array (ALMA) and the Submillimeter Array (SMA) of the three best-known Galactic red novae, V4332 Sgr, V1309 Sco, and V838 Mon. The observations were taken 22, 8, and 14yr after their respective eruptions and reveal the presence of molecular gas at excitation temperatures of 35-200K. The gas displays molecular emission in rotational transitions with very broad lines (full width ∼400km/s). We found emission of CO, SiO, SO, SO2 (in all three red novae), H2S (covered only in V838 Mon), and AlO (present in V4332 Sgr and V1309 Sco). No anomalies were found in the isotopic composition of the molecular material, and the chemical (molecular) compositions of the three red novae appear similar to those of oxygen-rich envelopes of classical evolved stars (RSGs, AGBs, post-AGBs). The minimum masses of the molecular material that was most likely dispersed in the red-nova eruptions are 0.05, 0.01, and 10–4M for V838 Mon, V4332 Sgr, and V1309 Sco, respectively. The molecular outflows in V4332 Sgr and V1309 Sco are spatially resolved and appear bipolar. The kinematic distances to V1309 Sco and V4332 Sgr are 2.1 and 4.2kpc, respectively. The kinetic energy stored in the ejecta of the two older red-nova remnants of V838 Mon and V4332 Sgr is of the order of 1046erg, similar to values found for some post-AGB (pre-PN) objects whose bipolar ejecta were also formed in a short-duration eruption. Our observations strengthen the link between these post-AGB objects and red novae and support the hypothesis that some of the post-AGB objects were formed in a common-envelope ejection event or its most catastrophic outcome, a merger.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: mass-loss - stars: individual: V1309 Sco - stars: individual: V4332 Sgr - stars: individual: V838 Mon - circumstellar matter - submillimeter: stars - astrochemistry

CDS comments: M31 LNR 2015 not identified.

Simbad objects: 31

goto Full paper

goto View the reference in ADS

Number of rows : 31

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 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10946 1
2 NAME NGC 300 OT2008-1 ev 00 54 34.16 -37 38 28.6           ~ 107 1
3 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1443 0
4 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4488 2
5 QSO B0605-0834 QSO 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 395 1
6 V* V838 Mon CV* 07 04 04.8222936785 -03 50 50.637499515   15.5   15.18 14.51 M10+B3V 373 0
7 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 998 0
8 QSO B0723-007 BLL 07 25 50.63996171 -00 54 56.5441985   17.39 16.57 15.82   ~ 217 1
9 QSO J0730-116 QSO 07 30 19.11247420 -11 41 12.6005110     20.30 20.3   ~ 262 1
10 QSO B0736+01 QSO 07 39 18.03389693 +01 37 04.6178588   16.90 16.47 16.19   ~ 624 1
11 OH 231.8 +4.2 OH* 07 42 16.947 -14 42 50.20           M10III+A 503 1
12 4C 01.28 BLL 10 58 29.60520747 +01 33 58.8237691   18.74 18.28 16.68   ~ 647 2
13 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5324 1
14 NAME Boomerang Nebula pA* 12 44 46.0900155125 -54 31 13.356991600       13.06   ~ 50 0
15 NAME M101 OT2015-1 SN? 14 02 16.78 +54 26 20.5   19.19 17.57 16.92 16.26 ~ 31 0
16 QSO B1730-130 QSO 17 33 02.70578476 -13 04 49.5481484   18 18.5 18.78 17.39 ~ 984 1
17 PMN J1733-3722 Rad 17 33 15.19301090 -37 22 32.3959728           ~ 37 1
18 IVS B1740-309 Rad 17 43 17.8884 -30 58 18.662           ~ 6 0
19 QSO J1744-3116 QSO 17 44 23.57824 -31 16 36.2943           ~ 118 1
20 V* V1309 Sco CV* 17 57 32.9383021931 -30 43 09.967391199   16.9   14.8   ~ 180 0
21 EWS 2002-BLG-360 CV* 17 57 38.98752 -29 46 05.1636           ~ 27 0
22 QSO J1832-2039 BLL 18 32 11.0447839878 -20 39 48.202176867   18.56 20.2     ~ 38 1
23 PMN J1838-1853 Rad 18 38 46 -18 53.7           ~ 2 0
24 PMN J1845-2200 Rad 18 45 39.90294845 -22 00 36.5735207           ~ 7 0
25 V* V4332 Sgr CV* 18 50 36.6959119600 -21 23 28.927014456         14.37 K8/M0e 144 0
26 QSO B1908-202 QSO 19 11 09.65289198 -20 06 55.1089891   18.21   18.14   ~ 235 0
27 QSO B1921-293 BLL 19 24 51.05595514 -29 14 30.1210524   18.71 18.21 15.07   ~ 690 0
28 Min 1-92 pA* 19 36 18.9292148675 +29 32 49.838032394 12.13 12.35 11.75 11.54   B0.5IV[e] 236 1
29 V* CK Vul CV* 19 47 37.9563868576 +27 18 41.788878128           ~ 108 0
30 IRAS 22036+5306 pA* 22 05 30.29 +53 21 32.8   19.2       F4III 74 0
31 PN KjPn 8 PN 23 24 10.472 +60 57 30.75           ~ 111 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018A&A...617A.129K and select 'bookmark this link' or equivalent in the popup menu


2020.08.04-22:16:30

© Université de Strasbourg/CNRS

    • Contact