V838 Monocerotis

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V838 Monocerotis
V838 Mon HST.jpg
V838 Monocerotis and its light echo as imaged by the Hubble Space Telescope on December 17, 2002. Credit: NASA/ESA
Observation data
Epoch 2000.0      Equinox 2000.0
Constellation Monoceros
Right ascension 07h 04m 04.85s
Declination −03° 50′ 50.1″
Apparent magnitude (V) 15.74
Astrometry
Distance 6,100[1] pc
Characteristics
Spectral type M6.3I[2]
Details
Radius 380[2] R
Luminosity 15,000[2] L
Temperature 3,270[2] K
Other designations
Nova Monocerotis 2002, GSC 04822-00039
Database references
SIMBAD data

V838 Monocerotis (V838 Mon) is a red variable star in the constellation Monoceros about 20,000 light years (6 kpc)[3] from the Sun. The previously unknown star was observed in early 2002 experiencing a major outburst, and was possibly one of the largest known stars for a short period following the outburst. Originally believed to be a typical nova eruption, it was then realized to be something completely different. The reason for the outburst is still uncertain, but several conjectures have been put forward, including an eruption related to stellar death processes and a merger of a binary star or planets.

The remnant is evolving rapidly. By 2009 its temperature had increased to 3,270K and its luminosity was 15,000 times solar, but its radius had decreased to 380 times that of the sun although the ejecta continues to expand.[2] The opaque ejected dust cloud has completely engulfed the B-type companion.

Outburst[edit]

On January 6, 2002, an unknown star was seen to brighten up in Monoceros, the Unicorn.[4] Being a new variable star, it was designated V838 Monocerotis, the 838th variable star of Monoceros. The initial light curve resembled that of a nova, an eruption that occurs when enough hydrogen gas has accumulated on the surface of a white dwarf from its close binary companion. Therefore it was also designated Nova Monocerotis 2002. V838 Monocerotis reached maximum visual magnitude of 6.75 on February 6, 2002, after which it started to dim rapidly, as expected. However, in early March the star started to brighten again, this time mostly in infrared wavelengths. Yet another brightening in infrared occurred in early April, after which the star returned to near its original brightness before the eruption, magnitude 15.6. The light curve produced by the eruption is unlike anything previously seen.[5]

The star brightened to about a million times solar luminosity[6] and absolute magnitude of −9.8,[1] ensuring that at the time of maximum V838 Monocerotis was one of the most luminous stars in the Milky Way galaxy. The brightening was caused by a rapid expansion of the outer layers of the star. The star was observed using the Palomar Testbed Interferometer, which provided a radius of 1,570 ± 400 solar radii (comparable to Jupiter's orbital radius), confirming the earlier indirect calculations.[7] The expansion took only a couple of months, meaning that its speed was abnormal. The laws of thermodynamics dictate that expanding gases cool. Therefore, the star became extremely cool and deep red. In fact, some astronomers argue that the spectra of the star resembled that of L-type brown dwarfs. If that is the case, V838 Monocerotis would be the first known L-type supergiant.[8] However, current estimates of the distance, and hence of the radius, are about 25% lower than assumed in those papers.[1]

Other possibly similar events[edit]

There are a handful of outbursts that resemble the one that occurred on V838 Monocerotis. In 1988, a red star was detected erupting in the Andromeda Galaxy. The star, designated M31-RV, reached the absolute bolometric magnitude of −9.95 at maximum (corresponding a luminosity of 0.75 million times solar) before dimming beyond detectability. A similar eruption occurred in 1994 in the Milky Way (V4332 Sagittarii).[9]

Progenitor star[edit]

Some details are emerging on the nature of the star that experienced the outburst. Based on an incorrect interpretation of the light echo the eruption generated, the distance of the star was first estimated to be 1,900 to 2,900 light years. Combined with the apparent magnitude measured from pre-eruption photographs, it was thought to be an underluminous F-type dwarf not much unlike our Sun, which posed a considerable enigma.[10]

More accurate measurements gave a much larger distance, 20,000 light years (6 kpc). It appears that the star is considerably more massive and luminous than the Sun. The star probably has a mass of from 5 to 10 times solar,[11] and a luminosity of from 550 to 5,000 times solar. The star may have originally had a radius roughly 5 times solar and temperature of 4,700–30,000 K.[3] Munari et al. (2005) suggest that the progenitor star is in fact a very massive supergiant with a mass of about 65 times solar. They also conclude that the system may be only about 4 million years old.[12]

The spectrum of V838 Monocerotis reveals a companion, a hot blue B-type main sequence star probably not much different from the progenitor star.[11] It is also possible that the progenitor was slightly less massive than the companion and only just entering the main sequence.[10]

Based on the photometric parallax of the companion, Munari et al. get a greater distance, 36,000 light years (10 kpc).[12]

Light echo[edit]

Images showing the expansion of the light echo. Credit: NASA/ESA.

Rapidly brightening objects like novae and supernovae are known to produce a phenomenon known as light echo. The light that travels directly from the object arrives first. If there are clouds of interstellar matter around the star, some light is reflected from the clouds. Because of the longer path, the reflected light arrives later, producing a vision of expanding rings of light around the erupted object.[5]

In the case of V838 Monocerotis, the light echo produced was unprecedented and is well documented in images taken by the Hubble Space Telescope. While the photos appear to depict an expanding spherical shell of debris, they are actually formed by the illumination of an ever-expanding ellipsoid with the progenitor star at one focus and the observer at the other. Hence, despite appearances, the structures in these photos are actually concave toward the viewer. In other words, the light is reflecting dust that is mostly 'behind' the star, not in 'front' of it.

It is not yet clear if the surrounding nebulosity is associated with the star itself. If that is the case, they may have been produced by the star in earlier eruptions which would rule out several models that are based on single catastrophic events.[5] However, there is strong evidence that the V838 Monocerotis system is very young and still embedded in the nebula from which it formed.[6]

Interestingly, the eruption initially emitted at shorter wavelengths (i.e. was bluer), which can be seen in the light echo: the outer border is bluish in the Hubble images.[5]

Models[edit]

So far several rather different explanations for the eruption of V838 Monocerotis have been published.

Atypical nova outburst[edit]

The outburst of V838 Monocerotis may be a nova eruption after all, albeit a very unusual one. However, this is very unlikely considering that the system includes a B-type star, and stars of this type are young and massive. There has not been enough time for a possible white dwarf to cool and accrete enough material to cause the eruption.[9]

Thermal pulse of a dying star[edit]

V838 Monocerotis may be a post-asymptotic giant branch star, on the verge of its death. The nebulosity illuminated by the light echo may actually be shells of dust surrounding the star, created by the star during previous similar outbursts. The brightening may have been a so-called helium flash, where the core of a dying low-mass star suddenly ignites helium fusion disrupting, but not destroying, the star. Such an event is known to have occurred in Sakurai's Object. However, several pieces of evidence support the argument that the dust is interstellar rather than centered around V838 Monocerotis. A dying star that has lost its outer envelopes would be appropriately hot, but the evidence points to a young star instead.[11]

Thermonuclear event within a massive supergiant[edit]

According to some evidence, V838 Monocerotis may be a very massive supergiant. If that is the case, the outburst may have been a so-called helium flash, a thermonuclear event where a shell in the star containing helium suddenly ignites and starts to fuse helium. Very massive stars survive multiple such events; however, they experience heavy mass loss (about half of the original mass is lost while in the main sequence) before settling as extremely hot Wolf-Rayet stars. This theory may also explain the apparent dust shells around the star. V838 Monocerotis is located in the approximate direction of the Galactic anticenter and off from the disk of the Milky Way. Stellar birth is less active in outer galactic regions, and it is not clear how such a massive star can form there. However, there are very young clusters like Ruprecht 44 and the 4-million-year-old NGC 1893 at a distance of ca. 7 kpc and 6 kpc, respectively.[12]

Mergeburst[edit]

The outburst may have been the result of a so-called mergeburst, the merger of two main sequence stars (or an 8 M main sequence star and a 0.3 M pre-main sequence star). This model is strengthened by the apparent youth of the system and the fact that multiple stellar systems may be unstable. The less massive component may have been in a very eccentric orbit or deflected towards the massive one. Computer simulations have shown the merger model to be plausible. The simulations also show that the inflated envelope would have come almost entirely from the smaller component. In addition, the merger model explains the multiple peaks in the light curve observed during the outburst.[6]

Planetary capture event[edit]

Another possibility is that V838 Monocerotis may have swallowed its giant planets. If one of the planets entered into the atmosphere of the star, the stellar atmosphere would have begun slowing down the planet. As the planet penetrated deeper into the atmosphere, friction would become stronger and kinetic energy would be released into the star more rapidly. The star's envelope would then warm up enough to trigger deuterium fusion, which would lead to rapid expansion. The later peaks may then have occurred when two other planets entered into the expanded envelope. The authors of this model calculate that every year about 0.4 planetary capture events occur in Sun-like stars in the Milky Way galaxy, whereas for massive stars like V838 Monocerotis the rate is approximately 0.5–2.5 events per year.[3]

See also[edit]

References[edit]

  1. ^ a b c Sparks, W. B.; Bond, H. E.; Cracraft, M.; Levay, Z.; Crause, L. A.; Dopita, M. A.; Henden, A. A.; Munari, U.; Panagia, N.; Starrfield, S. G.; Sugerman, B. E.; Wagner, R. M.; l. White, R. (2008). "V838 Monocerotis: A Geometric Distance from Hubble Space Telescope Polarimetric Imaging of Its Light Echo". The Astronomical Journal 135 (2): 605. arXiv:0711.1495. Bibcode:2008AJ....135..605S. doi:10.1088/0004-6256/135/2/605.  edit
  2. ^ a b c d e Tylenda, R.; Kamiński, T.; Schmidt, M.; Kurtev, R.; Tomov, T. (2011). "High-resolution optical spectroscopy of V838 Monocerotis in 2009". Astronomy & Astrophysics 532: A138. arXiv:1103.1763. Bibcode:2011A&A...532A.138T. doi:10.1051/0004-6361/201116858.  edit
  3. ^ a b c Retter, A.; Zhang, B.; Siess, L.; Levinson, A. (May 22, 2006). "The planets capture model of V838 Monocerotis: conclusions for the penetration depth of the planet/s". Monthly Notices of the Royal Astronomical Society. 1 370 (3): 1565. arXiv:astro-ph/0605552. Bibcode:2006MNRAS.370.1565C. doi:10.1111/j.1365-2966.2006.10579.x. 
  4. ^ Brown, N. J. (January 10, 2002). "IAU Circular No. 7785". Retrieved 10 August 2006. 
  5. ^ a b c d Bond, Howard E.; Henden, Arne; Levay, Zoltan G.; Panagia, Nino; Sparks, William B.; Starrfield, Sumner; Wagner, R. Mark; Corradi, R. L. M.; Munari, U. (March 27, 2003). "An energetic stellar outburst accompanied by circumstellar light echoes". Nature 422 (6930): 405–408. arXiv:astro-ph/0303513. Bibcode:2003Natur.422..405B. doi:10.1038/nature01508. PMID 12660776. 
  6. ^ a b c Soker, N.; Tylenda, R. (June 15, 2006). "Modelling V838 Monocerotis as a Mergeburst Object". arXiv:astro-ph/0606371 [astro-ph].
  7. ^ Lane, B. F.; Retter, A.; Thompson, R. R.; Eisner, J. A. (April 2005). "Interferometric Observations of V838 Monocerotis". The Astrophysical Journal (The American Astronomical Society) 622 (2): L137–L140. arXiv:astro-ph/0502293. Bibcode:2005ApJ...622L.137L. doi:10.1086/429619. 
  8. ^ Evans, A.; Geballe, T. R.; Rushton, M. T.; Smalley, B.; van Loon, J. Th.; Eyres, S. P. S.; Tyne, V. H. (August 2003). "V838 Mon: an L supergiant?". Monthly Notice of the Royal Astronomical Society (Royal Astronomical Society) 343 (3): 1054. Bibcode:2003MNRAS.343.1054E. doi:10.1046/j.1365-8711.2003.06755.x. 
  9. ^ a b Boschi, F.; Munari, U. (May 2004). "M 31-RV evolution and its alleged multi-outburst pattern". Astronomy & Astrophysics 418 (3): 869–875. arXiv:astro-ph/0402313. Bibcode:2004A&A...418..869B. doi:10.1051/0004-6361:20035716.  M31-RV - 0402313
  10. ^ a b Tylenda, R. (June 4, 2005). "Evolution of V838 Monocerotis during and after the 2002 eruption". Astronomy and Astrophysics 436 (3): 1009–1020. arXiv:astro-ph/0502060. Bibcode:2005A&A...436.1009T. doi:10.1051/0004-6361:20052800. 
  11. ^ a b c Tylenda, R.; Soker, N.; Szczerba, R. (October 2005). "On the progenitor of V838 Monocerotis". Astronomy and Astrophysics 441 (3): 1099–1109. arXiv:astro-ph/0412183. Bibcode:2005A&A...441.1099T. doi:10.1051/0004-6361:20042485. Retrieved 10 August 2006. 
  12. ^ a b c Munari, U.; Munari, U.; Henden, A.; Vallenari, A.; Bond, H. E.; Corradi, R. L. M.; Crause, L.; Desidera, S.; Giro, E.; Marrese, P. M.; Ragaini, S.; Siviero, A.; Sordo, R.; Starrfield, S.; Tomov, T.; Villanova, S.; Zwitter, T.; Wagner, R. M. (May 2, 2005). "On the distance, reddening and progenitor of V838 Mon". Astronomy and Astrophysics 434 (3): 1107–1116. arXiv:astro-ph/0501604. Bibcode:2005A&A...434.1107M. doi:10.1051/0004-6361:20041751. 

External links[edit]

Coordinates: Sky map 07h 04m 04.85s, +03° 50′ 50.1″