Origin of Dust Around V1309 Sco

Zhu, Chengliang; Wang, Zhaojun

doi:10.1088/0004-637x/777/1/23

Cited by 20 publications

(22 citation statements)

References 30 publications

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“…Dust could already have been present in V1309 Sco in 2008 just before the eruption (Tylenda et al 2011;McCollum et al 2014;Zhu et al 2013), but absent before 2008 (Nicholls et al 2013). As explained in the earlier studies, the dusty material formed sometime before the eruption and is likely confined to a disk seen almost edge on.…”

Section: Temporal Changesmentioning

confidence: 64%

Post-outburst spectra of a stellar-merger remnant of V1309 Scorpii: from a twin of V838 Monocerotis to a clone of V4332 Sagittarii

Kamiński

Mason

Tylenda

et al. 2015

A&A

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We present optical and infrared spectroscopy of V1309 Sco, an object that erupted in 2008 in a stellar-merger event. During the outburst, V1309 Sco displayed characteristics typical of red transients, a class of objects similar to V838 Mon. Our observations were obtained in 2009 and 2012, i.e. months and years after the eruption of V1309 Sco, and illustrate severe changes in the remnant, mainly in its circumstellar surroundings. In addition to atomic gas observed in earlier epochs, we identified molecular bands of TiO, VO, H 2 O, ScO, AlO, and CrO. The infrared bands of CrO we analyse are the first astronomical identification of the features. Over the whole period covered by our data, the remnant was associated with a cool ( 1000 K) outflow with a terminal velocity of about 200 km s −1 . Signatures of warmer atomic gas, likely to be still dissipating the energy of the 2008 outburst, dramatically decreased their brightness between 2009 and 2012. In addition, the source of optical continuum disappeared sometime before 2012, likely owing to the formation of new dust. The final stage of V1309 Sco's evolution captured by our spectra is an object remarkably similar to an older red transient, V4332 Sgr. In addition to providing a detailed view on the settling of the eruptive object, the observations presented here reinforce the conclusion that all the Galactic red transients are a manifestation of the same phenomenon, i.e. a stellar merger. The late spectra of V1309 Sco also suggest peculiarities in the chemical composition of the remnant, which still need to be explored.

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Section: Temporal Changesmentioning

confidence: 64%

Post-outburst spectra of a stellar-merger remnant of V1309 Scorpii: from a twin of V838 Monocerotis to a clone of V4332 Sagittarii

Kamiński

Mason

Tylenda

et al. 2015

A&A

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“…Post-merger infrared observations by Nicholls et al (2013), along with simulations by Nandez et al (2014), and dust modeling by Zhu et al (2013), proved that a great amount of matter was expelled during the merging event and was converted into dust grains soon after. Besides this, simulations of mergers whose primary component is a main-sequence massive star (Glebbeek et al 2013) yield a stellar product with a heliumenhanced core.…”

Section: Discussionmentioning

confidence: 94%

First detections of FS Canis Majoris stars in clusters

Fuente

Najarro

Trombley

et al. 2015

A&A

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Context. FS CMa stars are low-luminosity objects showing the B[e] phenomenon whose evolutionary state remains a puzzle. These stars are surrounded by compact disks of warm dust of unknown origin. Hitherto, membership of FS CMa stars to coeval populations has never been confirmed. Aims. The discovery of low-luminosity line emitters in the young massive clusters Mercer 20 and Mercer 70 prompts us to investigate the nature of such objects. We intend to confirm membership to coeval populations in order to characterize these emission-line stars through the cluster properties.

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“…In order to show the distribution of the ELM WDs and metal-poor MS in the sdAs, we use the method of binary population synthesis (BPS). Following Lü et al (2012), Zhu et al (2013), Lü et al (2017), Zhu et al (2017) and Wang et al (2018), we combined rapid binary star evolution code BSE (Hurley et al 2000(Hurley et al , 2002 and the calculation results from MESA to get the whole ELM WDs populations. As introduced above, we use MESA to obtain the populations of ELM WDs and the parameter space produced by RL channel.…”

Section: Basic Assumption Of Bps For Elm Wds In Dds and Metal-poor Msmentioning

confidence: 99%

The Formation of Subdwarf A-type Stars

Zhu

et al. 2019

ApJ

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Subdwarf A-type stars (sdAs) are objects that have hydrogen-rich spectra with surface gravity similar to that of hot subdwarf stars but effective temperature below the zero-age horizontal branch (ZAHB). They are considered to be metal-poor main sequence (MS) stars or extremely low-mass white dwarfs (ELM WDs). In this work, using the stellar evolution code, Modules for Experiments in Stellar Astrophysics (MESA), we investigate the sdAs formed both by the evolution of (pre-)ELM WDs in double degenerate systems (DDs) and metal-poor main sequence with the single evolution models. We find that both of the evolutionary tracks of ELM WDs and metal-poor MSs can explain the observation properties of sdAs. However, the proportion between these two populations are uncertain. In this work, we adopt the method of binary population synthesis of both ELM WDs in the disk and metal-poor MS in the halo to obtain the populations of ELM WDs and metal-poor MSs at different stellar population ages and calculate their proportions. We find that the proportion of metal-poor MSs to sdA population for a stellar population of 10 Gyr is ∼98.5 percent, which is consistent with the conclusion that most sdAs (>95 percent) are metal-poor MSs. And the proportion of ELM WDs (metal-poor MSs) to sdA population increases (decreases) from 0.1% (99.9%) to 20% (80%) with the stellar population ages from 5 to 13.7 Gyr.

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Origin of Dust Around V1309 Sco

Cited by 20 publications

References 30 publications

Post-outburst spectra of a stellar-merger remnant of V1309 Scorpii: from a twin of V838 Monocerotis to a clone of V4332 Sagittarii

Post-outburst spectra of a stellar-merger remnant of V1309 Scorpii: from a twin of V838 Monocerotis to a clone of V4332 Sagittarii

First detections of FS Canis Majoris stars in clusters

The Formation of Subdwarf A-type Stars

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