SIMP J013656.5+093347: Diferenzas entre revisións
Sen resumo de edición Etiqueta: edición de código 2017 |
Sen resumo de edición Etiqueta: edición de código 2017 |
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Liña 59: | Liña 59: | ||
| mag_ap_2_banda_an=H |
| mag_ap_2_banda_an=H |
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| mag_ap_2=12.771 ± 0.032 |
| mag_ap_2=12.771 ± 0.032 |
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| mag_ap_3_banda_an=K |
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| mag_ap_1_banda_an=K |
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| mag_ap_3=12.562 ± 0.024 |
| mag_ap_3=12.562 ± 0.024 |
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Revisión como estaba o 23 de agosto de 2021 ás 13:48
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Modelo:Starbox astrometry Modelo:Starbox detail Modelo:Starbox catalog Modelo:Starbox reference Modelo:Starbox end
SIMP J013656.5+093347 | |
Data de observación Época X2000 Equinoccio X2000 | |
---|---|
Constelación | Piscis |
Ascensión recta | 01h 36m 57s |
Declinación | +09° 33′ 47.3″ |
Características | |
Tipo espectral | T2.5[1] |
Magnitude aparente (J) | 13.455 ± 0.030 |
Magnitude aparente (H) | 12.771 ± 0.032 |
Magnitude aparente (K) | 12.562 ± 0.024 |
Astrometría | |
Movemento propio (μ) | RA: 10[2] mas/ano Dec.: 5[2] mas/ano |
Distancia | 1,150[4] al (352[3] pc) |
Detalles | |
Masa | 3[5] MXup |
Gravidade superficial (log g) | 3,5[5] |
Idade | 3[5] Ma |
Outras denominacións | |
Referencias en bases de datos | |
SIMBAD | datos |
SIMP J013656.5 +093347 (abbreviated SIMP0136) is a brown dwarf or planetary mass object[8] at 19.9 light-years from Earth in the constellation Pisces. It belongs to the spectral class T2.5[1] and its position shifts due to its proper motion annually by about 1.24 arcsec in the right ascension.[9]
This brown dwarf provided the first evidence for periodic variability flux variations among T dwarfs. This has been interpreted as a signature of weather patterns coming in and out of view over the object's 2.4h rotation period. The shape of this lightcurve evolves over timescales of days, which has been interpreted as a sign of evolution of the cloud patterns in its atmosphere.[10]
In 2017, it was announced that the object's mass may be as low as 12.7 Jupiter masses and might be considered a rogue planet rather than a brown dwarf as it seems to be a member of the relatively young, 200 million-year-old Carina-Near stellar moving group.[8][11][12]
In 2018, astronomers noted, "Detecting SIMP J01365663+0933473 with the VLA through its auroral radio emission, also means that we may have a new way of detecting exoplanets, including the elusive rogue ones not orbiting a parent star ... This particular object is exciting because studying its magnetic dynamo mechanisms can give us new insights on how the same type of mechanisms can operate in extrasolar planets - planets beyond our Solar System ... We think these mechanisms can work not only in brown dwarfs, but also in both gas giant and terrestrial planets."[12] During the observation with the VLA only one pulse was detected for SIMP0136.The magnetic flux of SIMP0136 was estimated to be 3.2 kG.[13]
Notas
- ↑ 1,0 1,1 Artigau; et al. (2009). "Photometric Variability of the T2.5 Brown Dwarf SIMP J013656.5+093347: Evidence for Evolving Weather Patterns". The Astrophysical Journal 701 (2): 1534–1539. Bibcode:2009ApJ...701.1534A. arXiv:0906.3514. doi:10.1088/0004-637X/701/2/1534. Parámetro descoñecido
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ignorado (Axuda) - ↑ 2,0 2,1 Erro no código da cita: Etiqueta
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- ↑ Peña Ramírez, K.; Zapatero Osorio, M. R.; Béjar, V. J. S.; Martin, E. L.; Rebolo, R. (2015). "Characterization of the known T-type dwarfs towards the σ Orionis cluster". Astronomy and Astrophysics 574: A118. Bibcode:2015A&A...574A.118P. arXiv:1411.3370. doi:10.1051/0004-6361/201424816.
- ↑ "Mysterious Object Might be First Extrasolar Planet Photographed". Silver Star Academy. Consultado o 08-02-2010.
- ↑ 5,0 5,1 5,2 Erro no código da cita: Etiqueta
<ref>
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- ↑ Kenyon, M. J.; Jeffries, R. D.; Naylor, Tim; Oliveira, J. M.; Maxted, P. F. L. (2005). "Membership, binarity and accretion among very low-mass stars and brown dwarfs of the σ Orionis cluster". Monthly Notices of the Royal Astronomical Society 356 (1): 89. Bibcode:2005MNRAS.356...89K. doi:10.1111/j.1365-2966.2004.08455.x.
- ↑ Burgasser, Adam J.; Geballe, T. R.; Leggett, S. K.; Kirkpatrick, J. Davy; Golimowski, David A. (2006). "A Unified Near-Infrared Spectral Classification Scheme for T Dwarfs". The Astrophysical Journal 637 (2): 1067. Bibcode:2006ApJ...637.1067B. doi:10.1086/498563.
- ↑ 8,0 8,1 Gagné, Jonathan; Faherty, Jacqueline K.; Burgasser, Adam J.; Artigau, Étienne; Bouchard, Sandie; Albert, Loïc; Lafrenière, David; Doyon, René; Bardalez-Gagliuffi, Daniella C. (2017-05-15). "SIMP J013656.5+093347 is Likely a Planetary-Mass Object in the Carina-Near Moving Group". The Astrophysical Journal 841 (1): L1. Bibcode:2017ApJ...841L...1G. ISSN 2041-8213. arXiv:1705.01625. doi:10.3847/2041-8213/aa70e2. Parámetro descoñecido
|s2cid=
ignorado (Axuda) - ↑ Gaia Collaboration (2018-08-01). "Gaia Data Release 2 - Summary of the contents and survey properties". Astronomy & Astrophysics (en inglés) 616: A1. ISSN 0004-6361. arXiv:1804.09365. doi:10.1051/0004-6361/201833051. Parámetro descoñecido
|s2cid=
ignorado (Axuda) - ↑ Modelo:Cite arxiv
- ↑ "Presto change-o! Brown dwarf star is now a planet". newatlas.com (en inglés). 2017-05-11. Consultado o 2018-08-07.
- ↑ 12,0 12,1 Starr, Michelle (3 August 2018). "There Is an Absolutely Gigantic Rogue Planet Wandering Our Galactic Neighbourhood". ScienceAlert.com. Consultado o 3 August 2018.
- ↑ Kao, Melodie M.; Hallinan, Gregg; Pineda, J. Sebastian; Stevenson, David; Burgasser, Adam (August 2018). "The Strongest Magnetic Fields on the Coolest Brown Dwarfs". Astrophysical Journal Supplement Series (en inglés) 237 (2): 25. Bibcode:2018ApJS..237...25K. ISSN 0067-0049. doi:10.3847/1538-4365/aac2d5. Parámetro descoñecido
|doi-access=
ignorado (Axuda)