2MASS J05352184−0546085

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2MASS J05352184−0546085
2MASS J05352184-0546085.tif
Artist's impression of the 2M0535-05 system
Observation data
Epoch J2000        Equinox J2000
Constellation Orion
Right ascension 05h 35m 21.84732s [1]
Declination −05° 46′ 08.5714″ [1]
Characteristics
Evolutionary stage brown dwarf
Spectral type M6.5±0.5 [2]
Apparent magnitude  (J)14.65±0.03 [3]
Apparent magnitude  (H)13.90±0.04 [3]
Apparent magnitude  (K)13.47±0.03 [3]
Variable type eclipsing binary
Astrometry
Proper motion (μ)RA: 1.960  mas/yr [1]
Dec.: -0.049  mas/yr [1]
Parallax (π)2.6730 ± 0.2658  mas [1]
Distance 1,200 ± 100  ly
(370 ± 40  pc)
Orbit [4]
Period (P)9.779556(19)  d
Semi-major axis (a)0.0407±0.0008  AU
Eccentricity (e)0.3216±0.0019
Inclination (i)88.49±0.06°
Argument of periastron (ω)
(secondary)		215.3±0.5°
Semi-amplitude (K1)
(primary)		18.61±0.55 km/s
Semi-amplitude (K2)
(secondary)		29.14±1.40 km/s
Details [4]
A
Mass 0.0572±0.0033  M☉
Radius 0.690±0.011  R☉
Surface gravity (log g)3.52±0.03  cgs
Temperature 2715±200  K
Rotation 3.293±0.001  d
Rotational velocity (v sin i)10 [2]  km/s
Age ~1  Myr
B
Mass 0.0366±0.0022  M☉
Radius 0.540±0.009  R☉
Surface gravity (log g)3.54±0.03  cgs
Temperature ~2850 [a]   K
Rotation 14.05±0.05  d
Rotational velocity (v sin i)<5 [2]  km/s
Age ~1  Myr
Other designations
V2384 Ori, 2MASS J05352184-0546085 [3]
Database references
SIMBAD data

2MASS J05352184-0546085, abbreviated to 2M0535-05 and also known by its variable star designation V2384 Orionis, is a young eclipsing binary brown dwarf system in the Orion Nebula, about 1,200 light-years (370 parsecs ) away. It was discovered in 2006 and was the first eclipsing brown dwarf system to be discovered, [5] [6] predating the discovery of the transiting brown dwarf CoRoT-3b in 2008.

Contents

Light curves for V2384 Orionis in three infrared bands. Representative error bars are shown in violet. Plotted from data published by Gomez Maqueo Chew et al. (2009) V2384OriLightCurve.png
Light curves for V2384 Orionis in three infrared bands. Representative error bars are shown in violet. Plotted from data published by Gómez Maqueo Chew et al. (2009)

The pair orbit each other with a period of 9.8 days, and are about 60 and 38 times the mass of Jupiter, respectively. The system is very young, at an age of about 1 million years, so the brown dwarfs have yet to cool; they are M-type objects with temperatures comparable to red dwarf stars, and they are inflated in size to over half the radius of the Sun. [4] [6] The primary is observed to rotate with a period of 3.3 days and the secondary 14 days, indicating that they have not yet become tidally locked to each other. [4]

Unexpectedly, the less massive (secondary) brown dwarf is the hotter of the pair. [6] [2] Possible explanations for this temperature reversal include the two brown dwarfs differing slightly in age; [2] strong magnetic fields on the primary inhibiting convection, [2] supported by the primary's observed fast rotation and strong hydrogen-alpha emission; [7] large starspots on the primary, [4] though this was found to be unsupported by evidence; [8] and tidal heating, which is unlikely to be solely responsible for the temperature reversal. [9]

No infrared excess that would indicate the presence of a circumstellar disk has been detected in this system. [10]

See also

Notes

  1. ↑ Derived from the primary temperature of 2715 K and the secondary/primary temperature ratio of 1.050

Related Research Articles

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References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 Stassun, Keivan G.; Mathieu, Robert D.; Valenti, Jeff A. (August 2007). "A Surprising Reversal of Temperatures in the Brown Dwarf Eclipsing Binary 2MASS J05352184-0546085". The Astrophysical Journal . 664 (2): 1154–1166. arXiv: 0704.3106 . Bibcode:2007ApJ...664.1154S. doi:10.1086/519231.
  3. 1 2 3 4 "V* V2384 Ori". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 8 May 2024.
  4. 1 2 3 4 5 6 Gómez Maqueo Chew, Yilen; Stassun, Keivan G.; Prša, Andrej; Mathieu, Robert D. (July 2009). "Near-infrared Light Curves of the Brown Dwarf Eclipsing Binary 2MASS J05352184-0546085: Can Spots Explain the Temperature Reversal?". The Astrophysical Journal . 699 (2): 1196–1208. arXiv: 0905.0491 . Bibcode:2009ApJ...699.1196G. doi:10.1088/0004-637X/699/2/1196.
  5. ↑ Stassun, Keivan G.; Mathieu, Robert D.; Valenti, Jeff A. (March 2006). "Discovery of two young brown dwarfs in an eclipsing binary system". Nature . 440 (7082): 311–314. Bibcode:2006Natur.440..311S. doi:10.1038/nature04570.
  6. 1 2 3 "Astronomers Measure Precise Mass of a Binary Brown Dwarf". hubblesite.org. STScI. 15 March 2006. Retrieved 8 May 2024.
  7. ↑ Reiners, A.; Seifahrt, A.; et al. (December 2007). "Detection of Strong Activity in the Eclipsing Binary Brown Dwarf 2MASS J05352184-0546085: A Possible Explanation for the Temperature Reversal". The Astrophysical Journal . 671 (2): L149 –L152. arXiv: 0711.0536 . Bibcode:2007ApJ...671L.149R. doi:10.1086/525255.
  8. ↑ Mohanty, Subhanjoy; Stassun, Keivan G. (October 2012). "High-resolution Spectroscopy during Eclipse of the Young Substellar Eclipsing Binary 2MASS 0535-0546. II. Secondary Spectrum: No Evidence that Spots Cause the Temperature Reversal". The Astrophysical Journal . 758 (1): 12. arXiv: 1208.0300 . Bibcode:2012ApJ...758...12M. doi:10.1088/0004-637X/758/1/12.
  9. ↑ Heller, R.; Jackson, B.; et al. (May 2010). "Tidal effects on brown dwarfs: application to the eclipsing binary 2MASS J05352184-0546085. The anomalous temperature reversal in the context of tidal heating". Astronomy and Astrophysics . 514: A22. arXiv: 1002.1246 . Bibcode:2010A&A...514A..22H. doi:10.1051/0004-6361/200912826.
  10. ↑ Mohanty, Subhanjoy; Stassun, Keivan G.; Mathieu, Robert D. (May 2009). "Circumstellar Environment and Effective Temperature of the Young Substellar Eclipsing Binary 2MASS J05352184-0546085". The Astrophysical Journal . 697 (1): 713–720. arXiv: 0903.1892 . Bibcode:2009ApJ...697..713M. doi:10.1088/0004-637X/697/1/713.

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