HD 104237

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HD 104237
DXChaLightCurve.png
A light curve for DX Chamaeleontis, plotted from Hipparcos data [1]
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Chamaeleon
Right ascension 12h 00m 05.087s [2]
Declination −78° 11′ 34.57″ [2]
Apparent magnitude  (V)6.58 [3] (6.59 to 6.70) [4]
Characteristics
Evolutionary stage Pre-main sequence
Spectral type A7.5Ve–A8Ve [5]
B−V color index 0.241±0.008 [3]
Variable type Irregular [4]
Astrometry
Proper motion (μ)RA: −39.284  mas/yr [2]
Dec.: −5.784  mas/yr [2]
Parallax (π)9.3805 ± 0.0427  mas [2]
Distance 348 ± 2  ly
(106.6 ± 0.5  pc)
Absolute magnitude  (MV)1.34 [3]
Orbit [6] [7]
Period (P)19.856±0.002 d
Semi-major axis (a)0.22±0.06  AU
Eccentricity (e)0.643±0.006
Inclination (i)17+12
−9°
Periastron epoch (T)2,451,647.539±0.003  HJD
Semi-amplitude (K1)
(primary)		17.8±0.2 km/s
Details
Component A
Mass 2.2±0.2 [7]   M☉
Radius 2.7±0.2 [7]   R☉
Luminosity 31 [8]   L☉
Temperature 8,450 [8]   K
Rotation 4.33717±0.00316 d [9]
Rotational velocity (v sin i)12±2 [5]  km/s
Age 2 [5]   Myr
Component B
Mass 1.4±0.3 [7]   M☉
Other designations
DX Cha, CD−77°528, GC  16412, HD  104237, HIP  58520, SAO  256895, PPM  371328, WDS J11596-7813C [10]
Database references
SIMBAD data

HD 104237 is a candidate multiple star system [11] in the southern constellation of Chamaeleon. It has the variable star designation DX Chamaeleontis, abbreviated DX Cha; HD 104237 is the stellar designation from the Henry Draper Catalogue . The system is dimly visible to the naked eye with an apparent visual magnitude that ranges from 6.59 down to 6.70. [4] It is located at a distance of approximately 348  light-years from the Sun based on parallax measurements. The system is positioned just 2′ to the north-east [12] of the 5th magnitude star Epsilon Chamaeleontis, [13] and is a member of the ε Cha association of co-moving stars. [11]

N. Houk and A. P. Cowley found a stellar classification of 'B/A peculiar' for this object in 1975. [14] The following year, K. G. Nehize catalogued it as a star displaying emission lines. [15] In 1988, J. Y. Hu and associates found it to be a candidate Herbig Ae/Be star. This is a class of pre-main sequence stars that recently formed from a molecular cloud. [12] In particular, the star displays an infrared excess associated with a dusty circumstellar shell, [16] and its spectrum closely resembles other Herbig Ae/Be stars such as AB Aurigae and HR 5999. [17] No characteristic molecular cloud was detected nearby, although there are small molecular clumps in the vicinity that may be the remains of a dissipating cloud. [12]

This is the optically brightest Herbig star known, making it a useful object for investigation. [5] Delta scuti-like pulsations have been detected with frequencies of 33.29 and 36.61 cycles per day. [6] It is an X-ray source with a luminosity of 2.69×1030  erg ·sec−1, which may originate in a hot corona. [8] DX Cha displays an ultraviolet excess, which indicates the star is still accreting matter at a rate of ≈ 10−8  M☉·yr−1. This inflow is generating a pair of jets emerging from the poles of the star. The circumstellar disk is being viewed from nearly edge on. [5]

Infrared observations in 1996 showed evidence of an infrared source located at an angular separation of 1″, [8] now designated component B. In 2003, optical observations combined with the Chandra X-ray Observatory indicated that five low mass, pre-main sequence objects lie within 5″, equivalent to a projected distance of 1,500  AU from the primary, component A. [18] At least two of these are T Tauri stars. [5] It is uncertain whether all of the nearby companions form a gravitationally bound system with the primary. [11] The close A/B pair display radial velocity variation that indicate this is a double-lined spectroscopic binary with a K-type secondary. [6]

Related Research Articles

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<span class="mw-page-title-main">Iota Centauri</span> Star in the constellation Centaurus

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<span class="mw-page-title-main">HD 100546</span> Star in the constellation Musca

HD 100546, also known as KR Muscae, is a pre-main sequence star of spectral type B8 to A0 located 353 light-years from Earth in the southern constellation of Musca. The star is surrounded by a circumstellar disk from a distance of 0.2 to 4 AU, and again from 13 AU out to a few hundred AU, with evidence for a protoplanet forming at a distance of around 47 AU.

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HD 178911 is a triple star system with an exoplanetary companion in the northern constellation of Lyra. With a combined apparent visual magnitude of 6.70, it is a challenge to view with the naked eye. The system is located at a distance of approximately 161 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −38 km/s.

HD 97048 or CU Chamaeleontis is a Herbig Ae/Be star 603 ly away in the constellation Chamaeleon. It is a variable star embedded in a dust cloud containing a stellar nursery, and is itself surrounded by a dust disk.

<span class="mw-page-title-main">Epsilon Chamaeleontis</span> Star in the constellation Chamaeleon

Epsilon Chamaeleontis, Latinized from ε Chamaeleontis, is a triple star located in the southern circumpolar constellation Chamaeleon. The primary and secondary have apparent magnitudes of 5.33 and 6.02, making them visible to the naked eye. Hipparcos parallax measurements place the system at a distance of 360 light years and is currently receding with a heliocentric radial velocity of 13 km/s.

<span class="mw-page-title-main">Eta Chamaeleontis</span> Star in the constellation Chamaeleon

Eta Chamaeleontis, Latinized from η Chamaeleontis, is a star in the constellation Chamaeleon. It has an apparent magnitude of about 5.5, meaning that it is just barely visible to the naked eye. Based upon parallax measurements, this star is located some 325 light-years light years away from the Sun.

Pi Chamaeleontis, its name Latinized from π Chamaeleontis, is a binary star system located in the southern circumpolar constellation of Chamaeleon. It is dimly visible to the naked eye with an apparent visual magnitude of 5.64. Parallax measurements by Hipparcos put the system approximately 135 light-years away. It is drifting closer with a radial velocity of −10 km/s.

Tau1 Eridani, Latinized from τ1 Eridani, is a binary star system in the constellation Eridanus. It has an apparent magnitude of 4.46, making it visible to the naked eye in suitably dark conditions. This is a spectroscopic binary with an orbital period of 958 days. It is located about 46 light years from the Earth. At present, the system is moving away from the Sun with a radial velocity of +26 km/s. About 305,000 years ago, perihelion passage was made at an estimated distance of 30.5 ly (9.35 pc).

<span class="mw-page-title-main">HD 21278</span> Binary star system in the constellation Perseus

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<span class="mw-page-title-main">9 Ceti</span> Star in the constellation Cetus

9 Ceti is a star in the equatorial constellation of Cetus. It has the variable star designation BE Ceti, while 9 Ceti is the Flamsteed designation. It has an apparent visual magnitude of 6.4, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun.

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.

<span class="mw-page-title-main">HD 53367</span> Binary star system in the constellation Monoceros

HD 53367 is a triple star system in the constellation of Monoceros. The primary star was identified as a variable Herbig Ae/Be star in 1989. Its companion, spectroscopically discovered in 2006, is a pre-main-sequence star star with an average separation of 1.7 AU. The star system is embedded in the extended nebula IC 2177.

<span class="mw-page-title-main">V1794 Cygni</span> FK Comae Berenices variable in the constellation Cygnus

V1794 Cygni is a single variable star in the northern constellation Cygnus. It has the identifier HD 199178 from the Henry Draper Catalogue; V1794 Cygni is its variable star designation. With an apparent visual magnitude of 7.24, it's too dim to be visible with the naked eye but can be seen with binoculars. V1794 is located at a distance of 367 light-years (113 pc) based on parallax measurements, but is drifting closer to the Sun with a radial velocity of −31 km/s. It lies superimposed over a region of faint nebulosity to the west of the North American Nebula.

<span class="mw-page-title-main">HD 150193</span> Young binary star system in the constellation Ophiuchus

HD 150193 is a binary star system in the constellation of Ophiuchus. The primary star was identified as a Herbig Ae/Be star with a strong solar wind, losing approximately a tenth of solar mass per million years. It does host a very small debris disk, likely due to disk truncation by the nearby stellar companion. The disk is inclined 38±9° to the plane of sky. It appears to be highly evolved and asymmetric, with indications of flattening and grains growth.

<span class="mw-page-title-main">EX Lupi</span>

EX Lupi is a young, single T-Tauri star in the southern constellation of Lupus. An irregular variable, it is the prototype of young, low-mass eruptive stars named EXors, 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. The low latitude of this star, at a declination of −40°, makes it difficult for northern observers to view. Based on parallax measurements, it is located at a distance of about 505 light years from the Sun. The star lies next to a gap in the Lupus cloud complex, a star forming region.

<span class="mw-page-title-main">CQ Tauri</span> Star in the constellation Taurus

CQ Tauri is a young variable star in the equatorial constellation of Taurus. It is too faint to be visible to the naked eye with an apparent visual magnitude that ranges from 8.7 to 12.25. The distance to this star is approximately 487 light years based on parallax measurements, and it is drifting further away with a radial velocity of ~23 km/s. It appears to be part of the T-association Tau 4. CQ Tauri lies close enough to the ecliptic to undergo lunar occultations.

HD 193373 is a solitary red hued star located in the equatorial constellation Delphinus. It has an apparent magnitude of 6.21, placing it near the limit for naked eye visibility. Parallax measurements place it 846 light years distant and it is currently receding with a heliocentric radial velocity of 22.7 km/s.

<span class="mw-page-title-main">DR Chamaeleontis</span> Binary star in the constellation Chamaeleon

DR Chamaeleontis, also known as HD 93237, is a star located in the southern circumpolar constellation Chamaeleon. The system has an average apparent magnitude of 5.97, allowing it to be faintly visible to the naked eye. DR Cha is located relatively far at a distance of 1,060 light years based on Gaia DR3 parallax measurements, but is receding with a poorly constrained heliocentric radial velocity of 18 km/s.

References

  1. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. 1 2 3 4 5 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.
  3. 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  4. 1 2 3 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. 1 2 3 4 5 6 Grady, C. A.; et al. (June 2004), "The Environment of the Optically Brightest Herbig Ae Star, HD 104237", The Astrophysical Journal, 608 (2): 809–830, Bibcode:2004ApJ...608..809G, doi: 10.1086/420763 , S2CID   120264519.
  6. 1 2 3 Böhm, T.; et al. (December 2004), "Spectroscopic monitoring of the Herbig Ae star HD 104237. I. Multiperiodic stellar oscillations", Astronomy and Astrophysics, 427 (3): 907–922, Bibcode:2004A&A...427..907B, doi: 10.1051/0004-6361:20041227 .
  7. 1 2 3 4 Garcia, P. J. V.; et al. (April 2013), "Pre-main-sequence binaries with tidally disrupted discs: the Brγ in HD 104237", Monthly Notices of the Royal Astronomical Society, 430 (3): 1839–1853, arXiv: 1301.0276 , Bibcode:2013MNRAS.430.1839G, doi: 10.1093/mnras/stt005 .
  8. 1 2 3 4 Skinner, S. L.; Yamauchi, S. (November 1996), "ASCA Observations of HD 104237 (A4e) and the Origin of X-Ray Emission from Herbig AE Stars", Astrophysical Journal, 471 (2): 987, Bibcode:1996ApJ...471..987S, doi: 10.1086/178026 , S2CID   123243719.
  9. ↑ Järvinen, S. P.; et al. (July 2019), "The two magnetic components in the Herbig Ae SB2 system HD 104237", Monthly Notices of the Royal Astronomical Society, 486 (4): 5499–5503, arXiv: 1905.05586 , Bibcode:2019MNRAS.486.5499J, doi: 10.1093/mnras/stz1212 .
  10. ↑ "DX Cha", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2022-05-31.
  11. 1 2 3 Dickson-Vandervelde, D. Annie; et al. (February 2021), "Gaia-based Isochronal, Kinematic, and Spatial Analysis of the ɛ Cha Association", The Astronomical Journal, 161 (2): 17, arXiv: 2011.06621 , Bibcode:2021AJ....161...87D, doi: 10.3847/1538-3881/abd0fd , S2CID   234354886, 87
  12. 1 2 3 Knee, L. B. G.; Prusti, T. (August 1996), "Molecular gas near HD 104237 and ɛ Chamaeleontis", Astronomy and Astrophysics, 312: 455–462, Bibcode:1996A&A...312..455K.
  13. ↑ Sinnott, Roger W.; Perryman, Michael A. C. (1997), Millennium Star Atlas, vol. 2, Sky Publishing Corporation and the European Space Agency, p. 1023, ISBN   0-933346-83-2.
  14. ↑ Houk, N.; Cowley, A. P. (1975), "Catalogue of two-dimensional spectral types for the HD stars", University of Michigan, I, Bibcode:1975mcts.book.....H.
  15. ↑ Henize, K. G. (April 1976), "Observations of southern emission-line stars", Astrophysical Journal Supplement Series, 30: 491–550, Bibcode:1976ApJS...30..491H, doi: 10.1086/190369 .
  16. ↑ Hu, J. Y.; et al. (January 1989), "Photometric and spectroscopic study of three candidate Herbig Ae/Be stars : HD 37411, HD 100546 and HD 104237", Astronomy and Astrophysics, 208: 213–218, Bibcode:1989A&A...208..213H.
  17. ↑ Hu, J. Y.; et al. (August 1991), "IUE observations of the bright Herbig AE star HD 104237", Astronomy and Astrophysics, 248: 150, Bibcode:1991A&A...248..150H.
  18. ↑ Feigelson, Eric D.; et al. (December 2003), "The ɛ Chamaeleontis Young Stellar Group and the Characterization of Sparse Stellar Clusters", The Astrophysical Journal, 599 (2): 1207–1222, arXiv: astro-ph/0309059 , Bibcode:2003ApJ...599.1207F, doi:10.1086/379365, S2CID   16407429.

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