Astronomy:2MASS J04070752+1546457
Coordinates: 
04h 07m 07.53s, +15° 24′ 45.54″
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 07m 07.527s[1] |
| Declination | +15° 46′ 45.540″[1] |
| Characteristics | |
| Spectral type | L3.5[2] |
| Apparent magnitude (G) | 20.704 ± 0.014[1] |
| Apparent magnitude (J) | 15.478 ± 0.058[1] |
| Apparent magnitude (H) | 14.354 ± 0.057[1] |
| Apparent magnitude (K) | 13.559 ± 0.038[1] |
| Astrometry | |
| Radial velocity (Rv) | 43.4 ± 2.1[2] km/s |
| Proper motion (μ) | RA: 61.250 ± 3.490[1] mas/yr Dec.: –53.130 ± 2.712[1] mas/yr |
| Parallax (π) | 27.4408 ± 1.7735[1] mas |
| Distance | 119 ± 8 ly (36 ± 2 pc) |
| Details[2] | |
| Mass | 0.064+0.009 −0.027 M☉ |
| Radius | 0.100+0.024 −0.008 R☉ |
| Surface gravity (log g) | 5.2 ± 0.4 cgs |
| Temperature | 1840 ± 210 K |
| Rotation | 1.23±0.01 h |
| Rotational velocity (v sin i) | 82.6 ± 0.2 km/s |
| Age | 0.8+11.2 −0.65 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
2MASS J04070752+1546457 (abbreviated to 2MASS J0407+1546) is a rapidly-rotating brown dwarf of spectral class L3.5, located in the constellation Taurus about 119 light-years from Earth. With a photometrically measured rotation period of 1.23 hours, it is one of the fastest-rotating known brown dwarfs announced by a team of astronomers led by Megan E. Tannock in March 2021. With a rotational velocity of over 80 km/s (50 mi/s), it is approaching the predicted rotational speed limit beyond which it would break apart due to centripetal forces. As a consequence of its rapid rotation, the brown dwarf is slightly flattened at its poles to a similar degree as Saturn, the most oblate planet in the Solar System.[3] Its rapid rotation may enable strong auroral radio emissions via particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs.[2]
Discovery
2MASS J0407+1546 was first catalogued as a point source in June 2003 by the Two Micron All-Sky Survey (2MASS) organized by the University of Massachusetts Amherst and the Infrared Processing and Analysis Center under the California Institute of Technology.[4] It was discovered to be a brown dwarf of the spectral class L3.5 by I. Neill Reid and collaborators, based on near-infrared spectra obtained in October 2005 with the Gemini North at the Mauna Kea Observatory, Hawaii. Their discovery and spectroscopic characterization of 430 ultracool dwarfs including 2MASS J0407+1546 was published in The Astronomical Journal in September 2008.[5]
Distance
The trigonometric parallax of 2MASS 1114−2618 was measured to be 27.4408±1.7735 milliarcseconds by the Gaia spacecraft in 2018, corresponding to a distance of 36.4 ± 2.4 parsecs (118.7 ± 7.8 ly).[1] This is in close agreement with Reid et al.'s spectrophotometric estimate of 33.1 ± 3.3 parsecs (108 ± 11 ly) in 2008, calculated from the object's spectral type and near-infrared absolute magnitude.[5]
Proper motion
From Gaia DR2, 2MASS J0407+1546 has a measured net proper motion of 81.0 mas/yr with position angle 139.06 degrees,[lower-alpha 1][lower-alpha 2] indicating motion in south-east direction on the sky.[1]
See also
- 2MASS J12195156+3128497 – L8 spectral class brown dwarf with a period of 1.14+0.03
−0.01 h - 2MASS J03480772−6022270 – T7 spectral class brown dwarf with a period of 1.080+0.004
−0.005 h
Notes
- ↑ The net proper motion is given by: [math]\displaystyle{ \mu = \sqrt{ {\mu_\delta}^2 + {\mu_\alpha}^2 \cdot \cos^2 \delta } \approx 81.0 }[/math] mas/yr, where [math]\displaystyle{ \mu_\alpha }[/math] and [math]\displaystyle{ \mu_\delta }[/math] are the components of proper motion in the RA and Dec, respectively.
- ↑ The position angle of proper motion is given by [math]\displaystyle{ \tan^{-1} \left (\frac{\mu_{\delta}}{\mu_{\alpha}} \right ) }[/math]
References
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 "2MASS J04070752+1546457 -- Brown Dwarf (M<0.08solMass)". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=2MASS+J04070752%2B1546457.
- ↑ 2.0 2.1 2.2 2.3 Tannock, Megan E.Expression error: Unrecognized word "etal". (March 2021). "Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-cool Dwarfs". The Astronomical Journal 161 (5): 224. doi:10.3847/1538-3881/abeb67. Bibcode: 2021AJ....161..224T.
- ↑ Cofield, Calla (7 April 2021). "Trio of Fast-Spinning Brown Dwarfs May Reveal a Rotational Speed Limit". Jet Propulsion Laboratory (NASA). https://www.jpl.nasa.gov/news/trio-of-fast-spinning-brown-dwarfs-may-reveal-a-rotational-speed-limit.
- ↑ Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
- ↑ 5.0 5.1 Reid, I. Neill; Cruz, Kelle L.; Kirkpatrick, J. Davy; Allen, Peter R.; Mungall, F.; Liebert, James; Lowrance, Patrick; Sweet, Anne (September 2008). "Meeting the Cool Neighbors. X. Ultracool Dwarfs from the 2MASS All-Sky Data Release". The Astronomical Journal 136 (3): 1290–1311. doi:10.1088/0004-6256/136/3/1290. Bibcode: 2008AJ....136.1290R.
External links
- Trio of Fast-Spinning Brown Dwarfs May Reveal a Rotational Speed Limit, Calla Cofield, Jet Propulsion Laboratory, 7 April 2021
- Western space scientists identify fastest-spinning "failed stars" ever found, Jeff Renaud, University of Western Ontario, 7 April 2021
- Caught Speeding: Clocking the Fastest-Spinning Brown Dwarfs, NOIRLab, 7 April 2021
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