Luminous red nova

V838 Monocerotis – a prototypic Luminous red nova

A luminous red nova (abbr. LRN, pl. luminous red novae, pl.abbr. LRNe) is a stellar explosion thought to be caused by the merging of two stars. They are characterised by a distinct red colour, and a light curve that lingers with resurgent brightness in the infrared. Luminous red novae are not to be confused with standard novae, explosions that occur on the surface of white dwarf stars.

Discovery

A small number of objects exhibiting the characteristics of luminous red novae have been observed over the last 30 years or so. The red star M31 RV in the Andromeda Galaxy flared brightly during 1988 and may have been a luminous red nova. In 1994, V4332 Sgr, a star in the Milky Way galaxy, flared similarly, and in 2002, V838 Mon followed suit and was studied quite closely.

The first confirmed Luminous Red Nova was the object M85 OT2006-1, in the Messier 85 galaxy. It was first observed during the Lick Observatory Supernova Search, and subsequently investigated by a team of astronomers from both U.C. Berkeley and Caltech. The team, led by Shrinivas Kulkarni confirmed its difference from known explosions such as novae and thermal pulses, and announced Luminous Red Novae as a new class of stellar explosion in a press release on May 23, 2007 and by publication in the journal Nature.

V1309 Scorpii is a luminous red nova that followed the merger of a contact binary in 2008.^[1]

In January 2015, a luminous red nova was observed in the Andromeda Galaxy.^[2]

On February 10, 2015, a luminous red nova was observed in the Pinwheel Galaxy by Dumitru Ciprian Vîntdevară from Planetarium and Astronomical Observatory of the Museum Vasile Parvan in Barlad, Romania.^[3]^[4]

Characteristics

A luminous red nova has the following observed characteristics:

The luminosity of the explosion is between that of a supernova (which is brighter) and a nova (dimmer).
The visible light lasts for weeks or months, and is distinctively red in colour, becoming dimmer and redder over time. As the visible light dims, the infrared light grows and also lasts for an extended period of time, usually dimming and brightening a number of times.
Infrared observations of M85 OT2006-1 have shown it to be quite cool for a star (slightly less than 1000 K). This may, or may not, be a characteristic shared by other luminous red novae.

Evolution

The team investigating M85 OT2006-1 believe it to have formed when two main sequence stars merged. (See the article on V838 Mon for further information on mergebursts and alternative possibilities.)

At the time the mergeburst occurs, the LRN appears to expand extremely rapidly, reaching thousands to tens of thousands of solar radii in only a few months. This would cause the object to cool, explaining the intriguing co-existence of a bright flash with a cool post-flash object.

Other viewpoints

Some astronomers believe it to be premature to declare a new class of stellar explosions based on such a limited number of observations. For instance, Pastorello et al. 2007^[5] explained that the event may be due to a type II-p supernova and Todd et al. 2008^[6] pointed out that supernovae undergoing a high level of extinction will naturally be both red and of low luminosity.

References

↑ Tylenda, R.; Hajduk, M.; Kamiński, T.; Udalski, A.; Soszyński, I.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Poleski, R.; Wyrzykowski, Ł.; Ulaczyk, K. (2011). "V1309 Scorpii: Merger of a contact binary". Astronomy & Astrophysics 528: 114. arXiv:1012.0163v2. Bibcode:2011A&A...528A.114T. doi:10.1051/0004-6361/201016221.
↑ "M31N 2015-01a - A Luminous Red Nova". The Astronomer's Telegram. Retrieved 2015-03-18.
↑ "PSN J14021678+5426205 in M 101". The Astronomer's Telegram.
↑ "http://www.rochesterastronomy.org/". Bright Supernova. External link in |title= (help)
↑ Pastorello, A.; Della Valle, M.; Smartt, S. J.; Zampieri, L.; Benetti, S.; Cappellaro, E.; Mazzali, P. A.; Patat, F.; Spiro, S.; Turatto, M.; Valenti, S. (2007). "A very faint core-collapse supernova in M85". Nature 449 (7164): 1. arXiv:0710.3753. Bibcode:2007Natur.449E...1P. doi:10.1038/nature06282.
↑ Thompson, Todd A.; Prieto, José L.; Stanek, K. Z.; Kistler, Matthew D.; Beacom, John F.; Kochanek, Christopher S. (2009). "A New Class of Luminous Transients and a First Census of their Massive Stellar Progenitors". The Astrophysical Journal 705 (2): 1364. arXiv:0809.0510. Bibcode:2009ApJ...705.1364T. doi:10.1088/0004-637X/705/2/1364.

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