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2MASS J05352184−0546085

Artist's impression of the 2M0535-05 system
Observation data Epoch J2000      Equinox J2000
Constellation	Orion
Right ascension	05 35 21.84732
Declination	−05° 46′ 08.5714″
Characteristics
Evolutionary stage	brown dwarf
Spectral type	M6.5±0.5
Apparent magnitude (J)	14.65±0.03
Apparent magnitude (H)	13.90±0.04
Apparent magnitude (K)	13.47±0.03
Variable type	eclipsing binary
Astrometry
Proper motion (μ)	RA: 1.960 mas/yr Dec.: -0.049 mas/yr
Parallax (π)	2.6730 ± 0.2658 mas
Distance	1,200 ± 100 ly (370 ± 40 pc)
Orbit
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
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 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 K
Rotation	14.05±0.05 d
Rotational velocity (v sin i)	<5 km/s
Age	~1 Myr
Other designations
V2384 Ori, 2MASS J05352184-0546085
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, predating the discovery of the transiting brown dwarf CoRoT-3b in 2008.

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. 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.

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

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

See also

• 2M1510, another eclipsing binary brown dwarf

Notes

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

References

1. ^ 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. ^ 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. ^ "V* V2384 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 May 2024.
4. ^ 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. ^ "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.

Further reading

• Mohanty, Subhanjoy; Stassun, Keivan G.; Doppmann, Greg W. (October 2010). "High-resolution Spectroscopy During Eclipse of the Young Substellar Eclipsing Binary 2MASS 0535-0546. I. Primary Spectrum: Cool Spots Versus Opacity Uncertainties". The Astrophysical Journal. 722 (2): 1138–1147. arXiv:1008.2304. Bibcode:2010ApJ...722.1138M. doi:10.1088/0004-637X/722/2/1138.

v t e Constellation of Orion
List of stars in Orion Orion in Chinese astronomy Orion molecular cloud complex Orion's Belt Orion's Sword
Stars	Bayer α (Betelgeuse) β (Rigel) γ (Bellatrix) δ (Mintaka) ε (Alnilam) ζ (Alnitak) η (Algjebba) θ A B C D E F G H θ ι (Hatysa) κ (Saiph) λ (Meissa) μ ν ξ ο ο π π π (Tabit) π π π ρ σ τ υ (Thabit) φ φ χ χ ψ ψ ω Flamsteed 5 6 (g) 11 13 14 (i) 15 16 (h) 18 21 22 (o) 23 (m) 27 (p) 29 (e) 31 32 (A) 33 35 38 42 (c) 45 49 (d) 51 (b) 52 55 56 57 59 60 63 64 66 68 69 (f) 71 72 (f) 73 74 (k) 75 (l) Variable S U W UX VV BF BM DN FU GW V380 V883 V1005 V1149 V1201 V1352 V2247 V2254 V2384 HR 1759 1763 1874 1887 1952 1988 2007 2024 2251 2275 HD 33636 34445 37320 37605 42618 43317 290327 Other 4U 0614+091 CVSO 30 CWISE J0506+0738 Gliese 179 Gliese 205 Gliese 208 Gliese 221 GJ 3379 HOPS 383 LP 658-2 PDS 110 S Ori 52 S Ori 70 WISE J0457−0207 WISE J0521+1025
Exoplanets HD 34445 b HD 37605 b HD 38529 b HD 290327 b
Star clusters	NGC 1662 1980 1981 2169 2175 2194 2202 Other Lambda Orionis Cluster Trapezium Cluster (θ)
Nebulae	NGC 1788 1999 2022 2023 2064 2067 2071 2174 Other Abell 12 Abell 13 Barnard 30 Becklin–Neugebauer Object Flame Nebula HH 1/2 HH 24-26 HH 34 HH 111 Horsehead Nebula IC 434 IC 2118 LDN 1641 McNeil's Nebula Messier 43 Messier 78 Orion Nebula
Galaxies	NGC 1683 1819 1924 2110 2119 Other 4C +09.17 CGCG 396-2 II Zwicky 28 PKS 0458-020 PKS 0528+134 TXS 0506+056
Astronomical events GRB 991216
Category

• Orion (constellation)
• Orion molecular cloud complex
• Eclipsing binaries
• M-type brown dwarfs
• 2MASS objects
• Objects with variable star designations
• Astronomical objects discovered in 2006