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EX Lupi is a young, single[2] T-Tauri star in the southern constellation of Lupus. An irregular variable,[8] it is the prototype of young, low-mass eruptive stars named EXors,[2] with EX Lupi being this object's variable star designation. At its minimal activity level, EX Lupi resembles a classical T-Tauri star of the M0 dwarf type.[9] The low latitude of this star, at a declination of −40°, makes it difficult for northern observers to view.[9] Based on parallax measurements, it is located at a distance of approximately 514 light years from the Sun.[1] The star lies next to a gap in the Lupus cloud complex, a star forming region.[10]

EX Lupi

Artist's illustration of the disk around EX Lupi, showing the formation of silicate crystals
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Lupus
Right ascension 16h 03m 05.491s[1]
Declination −40° 18′ 25.43″[1]
Characteristics
Evolutionary stage Pre-main-sequence[2]
Spectral type M0[3]
Variable type YY Ori[4]
Astrometry
Radial velocity (Rv)−0.9±0.1[2] km/s
Proper motion (μ) RA: −10.095 mas/yr[1]
Dec.: −22.536 mas/yr[1]
Parallax (π)6.3413 ± 0.0376 mas[1]
Distance514 ± 3 ly
(157.7 ± 0.9 pc)
Details
Mass0.6[2] M☉
Radius1.6[2] R☉
Luminosity1.23±0.53[3] L☉
Temperature3,850±177[3] K
Rotational velocity (v sin i)4.4±2.0[5] km/s
Other designations
EX Lup, HD 325367, IRAS 15597-4010,[6] HV 11976[7]
Database references
SIMBADdata

During 1944, Edith M. Janssen at Harvard Observatory noticed a stellar spectrum that displayed bright lines on a photographic plate taken April 11, 1929, but these lines were missing on a spectrum from July 13, 1928. This star was found to be only two magnitudes fainter than at maximum, so a nova was ruled out. D. B. McLaughlin then undertook a study of this object going as far back as 1893, finding further outbursts in 1901, 1914, 1925, 1929, 1934. Each time the brightness increased by about two magnitudes, followed by smaller, irregular fluctuations lasting 1–2 years before returning to a near constant minimum at magnitude 13.2.[7] Now designated EX Lupi, G. H. Herbig studied the spectrum of this irregular variable in 1950, finding that it is similar to other emission-line stars associated with nebulosity.[11]

The next observed outburst was during the period 1955–1957 and was tracked by A. F. Jones. It reached a peak magnitude of 8.4, followed by a secondary brightening about 300 days later.[9] After a period of quiescence during the 1980s, another eruptive burst was observed in March 1994.[8] It reached a peak magnitude of 11.5 on both April 30 and May 14.[9] The cause was now understood to be the result of a mass accretion event with the infalling matter releasing its kinetic energy on the T-Tauri star. This creates a hot emission region that dominates the light output from the star. Many of the emission lines show an inverse P Cygni profile, thereby demonstrating that it is coming from infalling material. Absorption lines in the spectrum show a redshift indicating a velocity of 300 km/s.[8]

A visual band light curve for EX Lupi, plotted from AAVSO data[12]
A visual band light curve for EX Lupi, plotted from AAVSO data[12]

A major outburst of EX Lupi began in January 2008,[13] and it reached a peak visual magnitude of 8 during February.[14] It remained optically brighter by five magnitudes for a period of seven months.[15] Infrared observations of the star's circumstellar disk during the outburst shows spectral features of crystalline silicates, including strong indications of forsterite. The features resembled those seen in comets and some protoplanetary disks. The temperature of the disk is mostly below 700 K, indicating a circumstellar dust-free inner hole with a radius of 0.2 AU.[14] The disk may extend outward to at least 150 AU. At stellar quiescence, the infrared silicate feature at a wavelength of 10 μm can be explained as amorphous silicates of olivine and pyroxene.[2]

Matter from the circumstellar disk is being accreted onto the star by means of accretion columns.[5] This column may be the cause of the 7.417 day radial velocity variations observed with this star. EX Lupi is accreting mass at a typical estimated rate of 3.6×10−8 M☉·yr−1, which can climb as high as 10−7 M☉·yr−1 during peak bursts.[3] Between outbursts, the star undergoes moderate variability of 1–2 magnitudes due to variations in the rate of accretion.[5]


See also



References


  1. Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. Sipos, N.; et al. (November 2009), "EX Lupi in quiescence", Astronomy and Astrophysics, 507 (2): 881–889, arXiv:0906.3168, Bibcode:2009A&A...507..881S, doi:10.1051/0004-6361/200911641, S2CID 14365820.
  3. Alcalá, J. M.; et al. (April 2017), "X-shooter spectroscopy of young stellar objects in Lupus. Accretion properties of class II and transitional objects", Astronomy & Astrophysics, 600: 42, arXiv:1612.07054, Bibcode:2017A&A...600A..20A, doi:10.1051/0004-6361/201629929, S2CID 119211262, A20.
  4. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  5. Sicilia-Aguilar, Aurora; et al. (August 2015), "Accretion dynamics of EX Lupi in quiescence. The star, the spot, and the accretion column", Astronomy & Astrophysics, 580: 33, arXiv:1505.08011, Bibcode:2015A&A...580A..82S, doi:10.1051/0004-6361/201525970, S2CID 54725281, A82.
  6. "HD 325367", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2022-01-29.
  7. McLaughlin, Dean B. (November 1946), "The nova-like variable star HV 11976", Astronomical Journal, 52: 109, Bibcode:1946AJ.....52..109M, doi:10.1086/105935.
  8. Lehmann, T.; et al. (August 1995), "The outburst of the T Tauri star EX LUPI in 1994", Astronomy and Astrophysics, 300: L9, arXiv:astro-ph/9506066, Bibcode:1995A&A...300L...9L.
  9. Herbig, G. H.; et al. (December 2001), "The 1993-1994 Activity of EX Lupi", The Publications of the Astronomical Society of the Pacific, 113 (790): 1547–1553, Bibcode:2001PASP..113.1547H, doi:10.1086/324420.
  10. Herbig, G. H. (June 2007), "EX Lupi: History and Spectroscopy", The Astronomical Journal, 133 (6): 2679–2683, Bibcode:2007AJ....133.2679H, doi:10.1086/517494.
  11. Herbig, George H. (October 1950), "The Spectra of Five Irregular Variable Stars", Publications of the Astronomical Society of the Pacific, 62 (367): 211, Bibcode:1950PASP...62..211H, doi:10.1086/126276.
  12. "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  13. Jones, A. F. A. L. (January 2008), Green, D. W. E. (ed.), "EX Lupi", Central Bureau Electronic Telegrams, 1217 (1): 1, Bibcode:2008CBET.1217....1J.
  14. Ábrahám, P.; et al. (May 2009), "Episodic formation of cometary material in the outburst of a young Sun-like star", Nature, 459 (7244): 224–226, arXiv:0906.3161, Bibcode:2009Natur.459..224A, doi:10.1038/nature08004, PMID 19444209, S2CID 4426934.
  15. Aspin, Colin; et al. (August 2010), "The 2008 Extreme Outburst of the Young Eruptive Variable Star EX Lupi", The Astrophysical Journal Letters, 719 (1): L50–L55, arXiv:1007.4178, Bibcode:2010ApJ...719L..50A, doi:10.1088/2041-8205/719/1/L50, S2CID 2670001.

Further reading



На других языках

[de] EX Lupi

EX Lupi ist ein veränderlicher Stern im Sternbild Wolf. Er ist der Prototyp einer Unterklasse der T-Tauri-Sterne, die als EXors oder EX-Lupi-Sterne bezeichnet werden und durch optische Ausbrüche von 1 bis 4 mag gekennzeichnet sind, die jeweils etwa zehn bis einhundert Tage dauern und im Abstand von mehreren Monaten bis Jahren erfolgen. Sie sind meist Zwerge der Spektralklassen K oder M. Wie alle T-Tauri-Sterne ist EX Lupi selbst auch jung, nur einige Millionen Jahre alt.
- [en] EX Lupi

[ru] EX Волка

EX Волка (лат. EX Lupi), HD 325367 — одиночная переменная звезда[7][8][9][10] в созвездии Волка на расстоянии приблизительно 514 световых лет (около 158 парсеков) от Солнца. Видимая звёздная величина звезды — от +14,3m до +8,5m[11]. Возраст звезды определён в среднем как около 2 млн лет[12].


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