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HL Tauri

From Wikipedia, the free encyclopedia
Not to be confused with HL Tau 76.
HL Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 31m 38.437s[3]
Declination +18° 13′ 57.65″[3]
Characteristics
Evolutionary stage Pre-main-sequence star
Spectral type Class K9
Apparent magnitude (V) 15.1
B−V color index 0.92
V−R color index 0.89
J−H color index 1.45
J−K color index 3.21
Variable type T Tauri
Astrometry
Proper motion (μ) RA: +8.0±6.0[4] mas/yr
Dec.: -21.8±5.8[4] mas/yr
Distance450[1] ly
(140 pc)
Database references
SIMBADdata

HL Tauri (abbreviated HL Tau) is a young T Tauri star[5] in the constellation Taurus, approximately 450 light-years (140 pc) from Earth[1] in the Taurus Molecular Cloud.[6] The luminosity and effective temperature of HL Tauri imply that its age is less than 100,000 years.[7] At apparent magnitude 15.1,[3] it is too faint to be seen with the unaided eye. It is surrounded by a protoplanetary disk marked by dark bands visible in submillimeter radiation that may indicate a number of planets in the process of formation.[2] It is accompanied by the Herbig–Haro object HH 150, a jet of gas emitted along the rotational axis of the disk that is colliding with nearby interstellar dust and gas.[8]

Protoplanetary disk

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Indications of a protoplanetary disk were first presented in 1975[5] with infrared spectral observations in wavelengths between 2 and 4 microns, which were made possible by the recent invention of the indium antimonide photovoltaic detector. Of 29 very young stars examined, only HL Tauri showed a strong absorption feature centered on the expected 3.07 micron absorption of ice particles, which authors attributed to the ν1, ν3, and 2ν2 vibrational frequencies of the O–H bond.[9] A 1982 survey identified HL Tauri as one of the most highly polarized T Tauri stars known, along with DG Tauri and V536 Aquilae.[10]

A gas disk was discovered by interferometric observation of carbon monoxide (CO) emissions in 1986.[11] Based on observation data in 1985 and 1986 from the Millimeter Wave Interferometer of the Owens Valley Radio Observatory, the circumstellar disk was estimated to have a mass between 0.01 M☉ and 0.5 M☉, with a best fit of 0.1 M☉, and a radius of about 200 AU. The temperature of the gas and grains of the disk are probably of the order of a few tens of kelvins. The gas was found to be bound to and in Keplerian rotation around a star with a mass of about 1 M☉.[12] Bipolar outflow of molecules such as carbon monoxide (CO) and diatomic hydrogen (H2) have been observed. The element iron has also been noted in the outflow in its Fe(II) oxidation state, also called Fe2+ or ferrous iron.[13]

An image of the protoplanetary disk made at submillimeter wavelengths by the Atacama Large Millimeter/submillimeter Array (ALMA) was made public in 2014, showing a series of concentric bright rings separated by gaps. The disk appeared much more evolved than would have been expected from the age of the system, which suggests that the planetary formation process may be faster than previously thought.[14] ALMA's Catherine Vlahakis said, "When we first saw this image we were astounded at the spectacular level of detail. HL Tauri is no more than a million years old, yet already its disc appears to be full of forming planets. This one image alone will revolutionize theories of planet formation."[14]

Stephens et al. (2014) suggest that the faster accretion rate might be due to the complex magnetic field of the protoplanetary disk.[6]

In 2024, water was found within the protoplanetary disk using the Atacama Large Millimeter Array (ALMA), containing 3.7 Earth oceans worth of water vapour.[15][16]

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References

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  1. ^ a b c Webb, Johnathan (6 November 2014). "Planet formation captured in photo". BBC News. Retrieved 6 November 2014.
  2. ^ a b Blue, Charles E. (6 November 2014). "Birth of Planets Revealed in Astonishing Detail in ALMA's 'Best Image Ever'" (Press release). National Radio Astronomy Observatory. Archived from the original on 6 November 2014. Retrieved 6 November 2014.
  3. ^ a b c "HL Tauri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 6 November 2014.
  4. ^ a b Kwon, Woojin; Looney, Leslie W.; Mundy, Lee G. (November 2011). "Resolving the Circumstellar Disk of HL Tauri at Millimeter Wavelengths". The Astrophysical Journal. 741 (1). 3. arXiv:1107.5275. Bibcode:2011ApJ...741....3K. doi:10.1088/0004-637X/741/1/3. S2CID 118525138.
  5. ^ a b Weintraub, David A.; Kastner, Joel H.; Whitney, Barbara A. (October 1995). "In Search of HL Tauri". The Astrophysical Journal Letters. 452 (2): L141–L145. Bibcode:1995ApJ...452L.141W. doi:10.1086/309720. S2CID 122562823.
  6. ^ a b Stephens, Ian W.; Looney, Leslie W.; Kwon, Woojin; Fernández-López, Manuel; Hughes, A. Meredith; et al. (October 2014). "Spatially resolved magnetic field structure in the disk of a T Tauri star". Nature. 514 (7524): 597–599. arXiv:1409.2878. Bibcode:2014Natur.514..597S. doi:10.1038/nature13850. PMID 25337883. S2CID 4396150.
  7. ^ Boss, A. P.; Morfill, G. E.; Tscharnuter, W. M. (1989). "Models of the Formation and Evolution of the Solar Nebula". In Atreya, S. K.; Pollack, J. B.; Matthews, M. S. (eds.). Origin and Evolution of Planetary and Satellite Atmospheres. The University of Arizona Press. p. 45. Bibcode:1989oeps.book.....A. ISBN 978-0-8165-1105-1.
  8. ^ "Jets, bubbles, and bursts of light in Taurus". European Space Agency. 6 November 2014. Photo release Heic1424. Retrieved 7 November 2014.
  9. ^ Cohen, Martin (November 1975). "Infrared Observations of Young Stars—VI: A 2- to 4-Micron Search for Molecular Features". Monthly Notices of the Royal Astronomical Society. 173 (2): 279–293. Bibcode:1975MNRAS.173..279C. doi:10.1093/mnras/173.2.279.
  10. ^ Bastien, Pierre (April 1982). "A linear polarization survey of T Tauri stars". Astronomy and Astrophysics Supplement Series. 48: 153–164. Bibcode:1982A&AS...48..153B.
  11. ^ Beckwith, S.; Sargent, A. I.; Scoville, N. Z.; Masson, C. R.; Zuckerman, B.; et al. (October 1986). "Small-scale structure of the circumstellar gas of HL Tauri and R Monocerotis". The Astrophysical Journal. 309: 755–761. Bibcode:1986ApJ...309..755B. doi:10.1086/164645.
  12. ^ Sargent, Anneila I.; Beckwith, Steven (December 1987). "Kinematics of the circumstellar gas of HL Tauri and R Monocerotis". The Astrophysical Journal. 323: 294–305. Bibcode:1987ApJ...323..294S. doi:10.1086/165827.
  13. ^ Takami, Michihiro; Beck, Tracy L.; Pyo, Tae-Soo; McGregor, Peter; Davis, Christopher (November 2011). "A Micro-Molecular Bipolar Outflow from HL Tauri". The Astrophysical Journal. 670 (1): L33–L36. arXiv:0710.1148. Bibcode:2007ApJ...670L..33T. doi:10.1086/524138. S2CID 17086864.
  14. ^ a b Vlahakis, Catherine; Rubens, Valeria Foncea; Hook, Richard (6 November 2014). "Revolutionary ALMA Image Reveals Planetary Genesis". European Southern Observatory. Retrieved 7 November 2014.
  15. ^ Facchini, Stefano; Testi, Leonardo; Humphreys, Elizabeth; Donckt, Mathieu Vander; Isella, Andrea; Wrzosek, Ramon; Baudry, Alain; Gray, Malcom D.; Richards, Anita M. S.; Vlemmings, Wouter (29 February 2024). "Resolved ALMA observations of water in the inner astronomical units of the HL Tau disk". Nature Astronomy. 8 (5): 587–595. arXiv:2403.00647. doi:10.1038/s41550-024-02207-w. PMC 11399093. PMID 39282476.
  16. ^ de Lazaro, Enrico (29 February 2024). "ALMA Detects Water Vapor in Protoplanetary Disk around Young Star". Science News. Retrieved 29 February 2024.
  17. ^ "A glowing jet from a young star". European Space Agency. 18 February 2013. Photo release Potw1307a.
  18. ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
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  • Media related to HL Tauri at Wikimedia Commons
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