Hubble Space Telescope image showing Eta Carinae and the bipolar Homunculus Nebula which surrounds the star. The Homunculus was partly created in an eruption of Eta Carinae, the light from which reached Earth in 1843. Eta Carinae itself appears as the white patch near the center of the image, where the 2 lobes of the Homunculus touch.
|Observation data |
Epoch J2000 Equinox J2000
|Right ascension||10h 45m 03.591s|
|Declination||−59° 41′ 04.26″|
|Apparent magnitude (V)||4.47 (February 2011)  |
-0.8 to 7.9
|Spectral type||WR pe|
|U−B color index||-0.45|
|B−V color index||0.61|
|Variable type||LBV binary or multiple star|
|Radial velocity (Rv)||−25.0 km/s|
|Proper motion (μ)||RA: −7.6 mas/yr |
Dec.: 1.0 mas/yr
|Absolute magnitude (MV)||-5.45 to -5.74|
|Radius||85–195  R☉|
|Luminosity||5 × 106(bolometric) L☉|
|Age||~ <3 × 106 years|
Eta Carinae (η Carinae or η Car) is a stellar system in the constellation Carina, about 7,500 to 8,000 light-years from the Sun. The system contains at least two stars, one of which is a Wolf-Rayet star. Its combined luminosity is about four million times that of the Sun and has an estimated system mass in excess of 100 solar masses. It is not visible north of latitude 30°N and is circumpolar south of latitude 30°S. Because of its mass and the stage of life, it is expected to explode in a supernova in the astronomically near future.
Eta Carinae has the traditional names Tseen She (from the Chinese 天社 [Mandarin: tiānshè] "Heaven's altar") and Foramen.
In Chinese, 海山 (Hǎi Shān), meaning Sea and Mountain, refers to an asterism consisting of η Carinae, s Carinae, λ Centauri and λ Muscae. Consequently, η Carinae itself is known as 海山二 (Hǎi Shān èr, English: the Second Star of Sea and Mountain.)
This stellar system is currently one of the most massive that can be studied in great detail. Until recently, Eta Carinae was thought to be the most massive single star, but in 2005 it was realised to be a binary system. The most massive star in the Eta Carinae multiple star system has more than 100 times the mass of the Sun. Other known massive stars are more luminous and more massive.
Stars in the mass class of Eta Carinae, with more than 100 times the mass of the Sun, produce more than a million times as much light as the Sun. They are quite rare — only a few dozen in a galaxy as big as the Milky Way. They are assumed to approach (or potentially exceed) the Eddington limit, i.e., the outward pressure of their radiation is almost strong enough to counteract gravity. Stars that are more than 120 solar masses exceed the theoretical Eddington limit, and their gravity is barely strong enough to hold in their radiation and gas.
Eta Carinae's chief significance for astrophysics is based on its giant eruption or supernova impostor event, which was observed around 1843. In a few years, Eta Carinae produced almost as much visible light as a supernova explosion, but it survived. Other supernova impostors have been seen in other galaxies, for example the possible false supernovae SN 1961v in NGC 1058 and SN 2006jc in UGC 4904, which produced a false supernova, noted in October 2004. Significantly, SN 2006jc was destroyed in a supernova explosion two years later, observed on October 9, 2006. The supernova impostor phenomenon may represent a surface instability or a failed supernova. Eta Carinae's giant eruption was the prototype for this phenomenon, and after nearly 170 years the star's internal structure has not fully recovered.
 Brightness variations
One remarkable aspect of Eta Carinae is its changing brightness. It is currently classified as a luminous blue variable (LBV) binary star due to peculiarities in its pattern of brightening and dimming.
When Eta Carinae was first catalogued in 1677 by Edmond Halley, it was of the 4th magnitude, but by 1730, observers noticed it had brightened considerably and was, at that point, one of the brightest stars in Carina. Subsequently it dimmed again and by 1782 it appeared to have reverted to its former obscurity. In 1820, it was observed growing in brightness again. By 1827, it had brightened more than tenfold and reached its greatest apparent brightness in April 1843. With a magnitude of −0.8, it was the second brightest star in the night-time sky (after Sirius at 8.6 light years away), despite its enormous distance of 7,000–8,000 light-years. (To put the relationship in perspective, the relative brightness would be like comparing a candle (representing Sirius) at 14.5 meters (48 feet) to another light source (Eta Carinae) about 10 kilometers (6.2 mi) away, which would appear almost as bright as the candle.)
Eta Carinae sometimes has large outbursts, the last of which appeared in 1841, at around the time of its maximum brightness. The reason for these outbursts is not yet known. The most likely possibility is believed to be that they are caused by built-up radiation pressure from the star's enormous luminosity. After 1843, Eta Carinae's appearance faded away and between about 1900 and 1940 it was only of the 8th magnitude, invisible to the naked eye. Eta Carinae's sudden and unexpected doubled brightness was seen in 1998–1999. In 2007, its light could easily be seen with the naked eye at brighter than magnitude 5.
In 2008, the formerly clockwork regularity of the dimming was upset. Following its 5.52-year cycle, the star would normally have started its next dimming appearance in January 2009, but the pattern was noticed starting early in July 2008 by the southern Gemini Observatory in La Serena, Chile. Spectrographic measurements showed an increase in blue light from superheated helium, which was formerly assumed to occur with the wind shock. However, if the cause is a binary star, it would be located too far away at this point in time for the wind to interact in so significant a fashion. There is some debate about the cause of the recent event.
In 2010, Duane Hamacher and David Frew from Macquarie University in Sydney showed that the Boorong Aboriginal people of northwestern Victoria, Australia witnessed the outburst of Eta Carinae in the 1840s and incorporated it into their oral traditions as Collowgulloric War, the wife of War (the Crow, pronounced "Waah", denoted by the star Canopus). This is the only definitive indigenous record of Eta Carinae's outburst identified in the literature to date.
 X-ray source
4U 1037-60 (A 1044-59) is Eta Carinae. Three structures around Eta Carinae are thought to represent shock waves produced by matter rushing away from the superstar at supersonic speeds. The temperature of the shock-heated gas ranges from 60 MK in the central regions to 3 MK on the horseshoe-shaped outer structure. "The Chandra image contains some puzzles for existing ideas of how a star can produce such hot and intense X-rays," says Prof. Kris Davidson of the University of Minnesota.
A "spectroscopic minimum", or "X-ray eclipse", appeared in 2003. Astronomers organized a large observing campaign which included every available ground-based (e.g. CCD optical photometry) and space observatory, including major observations with the Hubble Space Telescope, the Chandra X-ray Observatory, the INTEGRAL Gamma-ray space observatory, and the Very Large Telescope. Primary goals of these observations were to determine if, in fact, Eta Carinae is a binary star and, if so, to identify its companion star; to determine the physical mechanism behind the "spectroscopic minima"; and to understand their relation (if any) to the large-scale eruptions of the 19th century.
There is good agreement between the X-ray light curve and the evolution of a wind-wind collision zone of a binary system. These results were complemented by new tests on radio wavelengths.
Spectrographic monitoring of Eta Carinae showed that some emission lines faded every 5.52 years, and that this period was stable for decades. The star's radio emission, along with its X-ray brightness, also drop precipitously during these "events" as well. These variations, along with ultra-violet variations, suggest a high probability that Eta Carinae is actually a binary star in which a hot, lower-mass star revolves around η Carinae in a 5.52-year, highly eccentric elliptical orbit.
The ionizing radiation emitted by the secondary star in Eta Carinae is the major radiation source of the system. Much of this radiation is absorbed by the primary stellar wind, mainly after it encounters the secondary wind and passes through a shock wave. The amount of absorption depends on the compression factor of the primary wind in the shock wave. The compression factor is limited by the magnetic pressure in the primary wind. The variation of the absorption by the post-shock primary wind with orbital phase changes the ionization structure of the circumbinary gas, and can account for the radio light curve of Eta Carinae. Fast variations near periastron passage are attributed to the onset of the accretion phase.
 Future prospects
Because of their disproportionately high luminosities, very large stars such as Eta Carinae use up their fuel very quickly. Eta Carinae is expected to explode as a supernova or hypernova some time within the next million years or so. As its current age and evolutionary path are uncertain, however, it could explode within the next several millennia or even in the next few years. LBVs such as Eta Carinae may be a stage in the evolution of the most massive stars; the prevailing theory now holds that they will exhibit extreme mass loss and become Wolf-Rayet stars before they go supernova, if they are unable to hold their mass to explode as a hypernova.
More recently, another possible Eta Carinae analogue was observed — namely SN 2006jc, some 77 million light years away in UGC 4904, in the constellation of Lynx. Its brightened appearance was noted on 20 October 2004, and was reported by amateur astronomer Koichi Itagaki as a supernova. However, although it had indeed exploded, hurling 0.01 solar masses (~20 Jupiters) of material into space, it had survived, before finally exploding nearly two years later as a Mag 13.8 type Ib supernova, seen on 9 October 2006. Its earlier brightening was a supernova impostor event.
Due to the similarity between Eta Carinae and SN 2006jc, Stefan Immler of NASA's Goddard Space Flight Center suggests that Eta Carinae could explode in our lifetime or even in the next few years. However, Stanford Woosley of the University of California in Santa Cruz disagrees with Immler’s suggestion, and says it is likely that Eta Carinae is at an earlier stage of evolution, and that it still has several kinds of material left for nuclear fusion.
In NGC 1260, a spiral galaxy in the constellation of Perseus some 238 million light years from earth, another analogue star explosion was supernova SN 2006gy, observed on September 18, 2006. A number of astronomers modeling supernova events have suggested that the explosion mechanism for SN 2006gy may be very similar to the fate that awaits Eta Carinae.
| ||This article or section appears to contradict itself. Please see the talk page for more information. (January 2011)|
It is possible that the Eta Carinae hypernova or supernova, when it occurs, could affect Earth, about 7,500 light years away. It is unlikely, however, to affect terrestrial lifeforms directly, as they will be protected from gamma rays by the atmosphere, and from some other cosmic rays by the magnetosphere. The damage would likely be restricted to the upper atmosphere, the ozone layer, spacecraft, including satellites, and any astronauts in space, although a certain few  claim that radiation damage to the upper atmosphere would have catastrophic effects as well. At least one scientist has claimed that when the star explodes, "it would be so bright that you would see it during the day, and you could even read a book by its light at night". A supernova or hypernova produced by Eta Carinae would probably eject a gamma ray burst (GRB) out on both polar areas of its rotational axis. Calculations show that the deposited energy of such a GRB striking the Earth's atmosphere would be equivalent to one kiloton of TNT per square kilometer over the entire hemisphere facing the star with ionizing radiation depositing ten times the lethal whole body dose to the surface. This catastrophic burst would probably not hit Earth, though, because the rotation axis does not currently point towards our solar system. If Eta Carinae is a binary system, this may affect the future intensity and orientation of the supernova explosion that it produces, depending on the circumstances.
 See also
- Homunculus Nebula
- LBV 1806-20
- Pistol Star
- SN 2006gy
- List of most luminous stars
- List of largest stars
- List of most massive stars
- Bipolar outflow
- ^ a b c d e "SIMBAD query result: V* eta Car -- Variable Star". Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Eta+Carinae. Retrieved 2008-04-25. —some of the data is located under "Measurements".
- ^ a b c Eduardo Fernández Lajús. "Optical monitoring of Eta Carinae". Universidad Nacional de La Plata. http://etacar.fcaglp.unlp.edu.ar/. Retrieved 2010-02-11.
- ^ a b "GCVS Query=Eta+Car". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. http://www.sai.msu.su/gcvs/cgi-bin/search.cgi?search=Eta+Car. Retrieved 2010-11-24.
- ^ "Eta Carinae: New View of Doomed Star". Chandra X-ray Center. http://chandra.harvard.edu/photo/2007/etacar/. Retrieved 2008-04-25.
- ^ http://etacar.umn.edu/etainfo/basic/
- ^ "VIZIER Details for Eta Carinae in Gould's Uranomatria Argentina". Centre de Données astronomiques de Strasbourg. http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=V/135/catalog&recno=1428. Retrieved 2011-02-14.
- ^ Davidson, Kris; Humphreys, Roberta (1997). "Eta Carinae and its Environment". Annual Review of Astronomy and Astrophysics 35 (1): 1–32. doi:10.1146/annurev.astro.35.1.1.
- ^ Kostjuk N.D.: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index 2002, refer to "table3.dat", the name "Foramen" somehow originating from ref #24: Rak I.V., Kholshevnikov K.V., Atlas Zvezdnogo neba, Sankt-Peterburg, "Neva", 1995
- ^ (Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
- ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 28 日
- ^ a b c Nancy Neal-Jones, Bill Steigerwald, "NASA Satellite Detects Massive Star Partner", NASA Goddard Space Flight Center, 1 November 2005
- ^ Stockdale, Christopher J.; Rupen, Michael P.; Cowan, John J.; Chu, You-Hua; Jones, Steven S. (2001). "The fading radio emission from SN 1961v: evidence for a Type II peculiar supernova?". The Astronomical Journal 122 (1): 283. arXiv:astro-ph/0104235. Bibcode 2001AJ....122..283S. doi:10.1086/321136.
- ^ Robert Naeye, "Supernova Impostor Goes Supernova", NASA Goddard Space Flight Center, 4 April 2007
- ^ Shiga, D. (2007). "Star's odd double explosion hints at antimatter trigger". New Scientist 2598 (2626): 18. doi:10.1016/S0262-4079(07)62628-1. http://space.newscientist.com/article.ns?id=dn11563&feedId=online-news_rss20.
- ^ see various articles in R.M. Humphreys & K.Z. Stanek (eds.) (2005). "The Fate of the Most Massive Stars". ASP Conference 332. Astronomical Society of the Pacific.
- ^ " Historical light curve"
- ^ a b Courtland, Rachel. "'Supernova impostor' begins to dim unexpectedly", NewScientist news service, 7 August 2008
- ^ Hamacher, D. W.; Frew, D. J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae". Journal of Astronomical History and Heritage 13 (3): 220–234. arXiv:1010.4610. Bibcode 2010arXiv1010.4610H.
- ^ "Chandra Takes X-ray Image of Repeat Offender". http://science.nasa.gov/newhome/headlines/ast08oct99_1.htm.
- ^ Falceta-Gonçalves, D.; Jatenco-Pereira, V.; Abraham, Z. (2005). "Wind-wind collision in the η Carinae binary system: a shell-like event near periastron". MNRAS 357 (3): 895. arXiv:astro-ph/0404363. Bibcode 2005MNRAS.357..895F. doi:10.1111/j.1365-2966.2005.08682.x.
- ^ Damineli, A. (1996). "The 5.52 Year Cycle of Eta Carinae". ApJ 460 (1): L49. Bibcode 1996ApJ...460L..49D. doi:10.1086/309961.
- ^ Stephen White, "Radio outburst of Eta Carinae", Department of Astronomy, University of Maryland College Park
- ^ Michael Corcoran, "RXTE X-ray lightcurve", Goddard Space Flight Center, last updated 10 December 2008
- ^ Kashi, A.; Soker, N. (2007). "Modelling the Radio Light Curve of Eta Carinae". Monthly Notices of the Royal Astronomical Society 378 (4): 1609. arXiv:astro-ph/0702389. Bibcode 2007astro.ph..2389K. doi:10.1111/j.1365-2966.2007.11908.x.
- ^ Smith, Nathan; Owocki, Stanley P. (2006). "On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars". The Astrophysical Journal 645 (1): L45. arXiv:astro-ph/0606174. Bibcode 2006ApJ...645L..45S. doi:10.1086/506523.
- ^ Robert S. (2007). "Massive star burps, then explodes". UC Berkeley News. http://www.berkeley.edu/news/media/releases/2007/04/04_supernova.shtml.
- ^ "Star dies in monstrous explosion", BBC News, 8 May 2007
- ^ Arnon Dar, A. De Rujula. "The threat to life from Eta Carinae and gamma ray bursts" Astrophysics and Gamma Ray Physics in Space, Series Vol. XXIV (2002), pp. 513-523
|Wikimedia Commons has media related to: Eta Carinae|
- Variable Star Of The Month AAVSO. April, 2000: Eta Carinae
- 'ETA CARINAE — an evolved triple-star system?' by Wolfgang Kundt and Christoph Hillemanns
- HST Treasury Project and General Information on Eta Carinae
- Eta Carinae profile
- Is there a "clock" in Eta Carinae? - Brazilian research about the star
- Broad Band Optical Monitoring
- X-ray Monitoring by RXTE
- Possible Hypernova could affect Earth
- ESO press release about the possibility of a supernova in 10 to 20 millennia
- The 2003 Observing Campaign
- Davidson et al., Kris (1999). "An Unusual Brightening Of Eta Carinae". The Astronomical Journal. http://adsabs.harvard.edu/abs/1999AJ....118.1777D. Retrieved 2007-04-08.
- Nathan, Smith (1998). "The Behemoth Eta Carinae: A Repeat Offender". Astronomical Society of the Pacific. http://www.astrosociety.org/pubs/mercury/9804/eta.html. Retrieved 2006-08-13.
- Eta Carinae at SIMBAD