L dwarf

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An object with the spectral type L (also called L-dwarf) can be either a low-mass star, [1] a brown dwarf [2] or a young free-floating planetary-mass object. [3] If a young exoplanet or planetary-mass companion is detected via direct imaging, it can also have an L spectral type, such as Kappa Andromedae b. [4]

Contents

Spectral characteristics

Spectrum of Kelu-1 (L-type binary, bottom line) in comparison to an M6-dwarf, which shows much stronger TiO and sodium absorption. The spectrum of the brown dwarf KELU-1 (eso9709b).jpg
Spectrum of Kelu-1 (L-type binary, bottom line) in comparison to an M6-dwarf, which shows much stronger TiO and sodium absorption.

Before 2MASS there were only six known objects with a spectral type later than M9.5V. With the discovery of 20 new late-type objects it was necessary to define the L-type and T-type spectral types. Kirkpatrick et al. defined the two spectral types in 1999. In these L-dwarfs the metallic oxides (TiO, VO), which are present in late M-dwarfs, are replaced with metallic hydrides (e.g. CrH, FeH) and neutral alkali metals (e.g. K, Rb, Cs). The transition between L- and T-dwarfs is defined with the appearance of methane (CH4) in the spectrum. [5] M-dwarfs show absorption due to water vapor (H2O) in their near-infrared spectrum. This absorption feature gets stronger with later L spectral type. The absorption due to carbon monoxide (CO) does show little variation over spectral type. [6] CO is replaced by CH4 in T-dwarfs. [7] Initially it was estimated that the hottest L0-dwarfs have a temperature of around 2000 K and the coldest L8-dwarfs have a temperature of about 1500 K. [5] Modern estimates range from 1100 K for L9, to a maximum of 2500 K for L0. [8] [9]

L-dwarfs have a red, violet or purple color due to absorption from the sodium D-line, which is centered at 5890 Å, overlapping with the color green. [7] Later work described L-dwarfs as having a violet color. [10]

Subdwarfs

Subdwarfs are objects with a low metallicity. These objects are usually old and their metallicity influences different absorption features. In particular, the collision induced absorption of hydrogen molecules leads to a suppression of the H- and K-band, which causes L-type subdwarfs to have blue near-infrared colors. 2MASS J0532+8246 was the first L-type subdwarf discovered. The prefix sd, esd and usd indicate subdwarfs, extreme subdwarfs and ultra subdwarfs. Objects with an usd-prefix have the lowest metallicity. [11]

Main-sequence stars

The hydrogen burning minimum mass lies at 0.075 M☉ (78.5 MJ) for objects with a solar metallicity. [12] The table of ultracool fundamental parameters lists several objects with an infrared spectral type of L0 to L4 and a mass above 78.5 MJ. One of the highest mass L-dwarfs in this list is G 239-25B (L0) for which they find a mass of 88.9 ±0.59 MJ. [8] [9] The hydrogen burning-limit is dependent on metallicity and objects with a low metallicity can have a higher hydrogen burning limit. Another factor is that a lower metallicity causes the atmosphere to be more transparent. Therefore older objects have temperatures that are higher. [13] Old L-subdwarfs with an early L spectral type can be main-sequence stars. [14] The brown dwarf SDSS J0104+1535 (usdL1.5, 0.086 ± 0.0015 M☉) for example is just below the hydrogen burning limit of around 0.088 M☉, for its metallicity of [Fe/H] = -2.4 ± 0.2. [13] The same team found that ⅓ of known L-subdwarfs are substellar objects and ⅔ are low-mass stars. [1] CWISE J1249+3621 (sdL1, 0.082+0.002
−0.003M☉) is for example a star, because the hydrogen burning limit is at around 0.080 for [M/H]=-1. This star is also a hypervelocity star. [14]

Brown dwarfs

Most L-dwarfs are brown dwarfs. Brown dwarfs are objects with a mass below 78.5 MJ. [12] Objects with a mass below 14 MJ are often referred to as planetary-mass objects, [15] but depending on their formation mechanism they are also called planetary-mass brown dwarfs. [16]

In the table of ultracool fundamental parameters there are currently 422 objects with an infrared spectral type of L and a mass range of 14-78.5 MJ. [8] [9] Additionally there are dozens of L-type brown dwarfs known that co-move with a star, white dwarf or brown dwarf. [2] The first L-type brown dwarf discovered was GD 165B, which orbits a white dwarf. [17] Its mass was later determined to be 62.58 ± 15.57 MJ. [18]

Planetary-mass objects and exoplanets

Free-floating planetary-mass object PSO J318.5-22, which is an L-dwarf PSO J318.5-22 image from the Pan-STARRS1 telescope.png
Free-floating planetary-mass object PSO J318.5−22, which is an L-dwarf

A planetary-mass object is commonly defined as an object with a mass below 14 MJ. These objects can be free-floating [15] or co-move with a star or brown dwarf (e.g. HD 106906 b). [19] [20] If such an object orbits a star within about 100 AU, it is referred to as an exoplanet. Beyond 100 AU, it is referred to as a planetary-mass companion since theories predict that these objects form on their own and not from material of a protoplanetary disk. [21] One exoplanet near this 100 AU boundary is Delorme 1 (AB)b, which could have formed via fragmentation of the circumstellar disk and is therefore considered an exoplanet. [22] More close-in planets, such as the planets around HR 8799 [23] and Kappa Andromedae b also resemble L-dwarfs or have an L spectral type. [4]

These objects are usually identified by their young age. An object can for example be present in a young star cluster (e.g. NGC 1333) [24] or a young association (see List of nearby associations). Researchers can use the temperature-age or luminosity-age relation to determine if its mass is below 13 MJ. [15] For very young star clusters (<1 Myr) even an L0 spectral type corresponds to a planetary-mass and therefore all L-dwarfs in such a star cluster have a planetary-mass. [24]

Another method is to determine other indicators of a young age. A lower-mass object has for example a lower surface gravity, which leads to a more extended atmosphere and more vertical mixing. This will affect the depth of certain spectral features and can lead to red near-infrared colors. A low-gravity L-dwarf is often denoted with the suffix β, γ and δ, indicating intermediate (β), low (γ) and very low (δ) gravity. Low-gravity L3-L5 dwarfs can also show lithium absorption. The so-called "lithium test" is less reliable to determine a low mass for young L-dwarfs. [25] An example for a low gravity object is CWISE J0506+0738, which has a spectral type between L8γ and T0γ and probably a mass of 7±2 MJ. [15]

Variability and clouds

Iron clouds with silicate clouds on top of it were theorized since the early 2000s for L-dwarfs. [26] The presence of silicates in L-dwarfs is well established with Spitzer observations. Especially L4-L6 dwarfs often show silicate absorption. But silicate absorption can also be absent for any L-dwarf. [27] Variability is often connected to the presence of clouds in L- and T-dwarfs. There are however other possible explanations, such as hot spots, temperature variations and aurorae. Especially young objects show variability. [28] One of the most variable L-dwarf is the planetary-mass companion VHS J1256–1257 b (L7), with an amplitude of 33-38%. [29]

Magnetic field and aurorae

Radio emission can be detected in L-dwarfs and this radio emission sometimes shows rotational periodic radio pulses. Additionally the H-alpha emission seen commonly in L-dwarf is interpreted as chromospheric and coronal in early L-dwarfs, but with later spectral type it will become more and more an auroral feature. Therefore L4-T8 objects with H-alpha emission are often also radio sources. Radio pulses from brown dwarfs are highly circular polarized and likely come from electron cyclotron maser instability (ECMI), which is connected to aurorae. It is currently not known what powers auroral radio emission in brown dwarfs. One suggestion is the breakdown of the co-rotation with a plasma disk, which also powers the main aurora on Jupiter. The other suggested energy source is the interaction with a rocky planet around the brown dwarf, similar to the interaction between Io and Jupiter. Impacts of electrons with hydrogen molecules can create a trihydrogen cation (H+
3). This could be detected in the infrared at 2 and 4 μm with JWST. Destruction of H+
3 by gases, such as H2O and CH4, could mean that it is not built up significantly in brown dwarfs. [30] No H+
3 was detected in any M, L or T dwarf with the Keck Observatory, likely due to auroral electrons penetrating deeper into the brown dwarf atmospheres and being destroyed by gases. [31] [32] The first L-dwarf with radio emission was 2MASS J00361617+1821104 (L3.5). [33]

Binaries

The L-type binary CWISE J0146-0508AB (L4+L8 blue) CWISE J0146-0508AB legacy dr10.jpg
The L-type binary CWISE J0146-0508AB (L4+L8 blue)

L-dwarfs are less often binaries than M-dwarfs. Systems with an L-dwarf as a primary have a binary fraction of 24+6
−2% with a typical separation of 5–8 astronomical units (AU). [35] There are also L-dwarfs with a wider separation, such as WISE 2150−7520 (L1+T8), which has a separation of 341 AU. [36] The closest L-dwarf to the Solar System is the primary in the Luhman 16 AB binary. It has a spectral type of L8. [37]

See also

Related Research Articles

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References

  1. 1 2 Zhang, Z. H.; Galvez-Ortiz, M. C.; Pinfield, D. J.; Burgasser, A. J.; Lodieu, N.; Jones, H. R. A.; Martín, E. L.; Burningham, B.; Homeier, D.; Allard, F.; Zapatero Osorio, M. R.; Smith, L. C.; Smart, R. L.; López Martí, B.; Marocco, F. (2018-11-01). "Primeval very low-mass stars and brown dwarfs - IV. New L subdwarfs, Gaia astrometry, population properties, and a blue brown dwarf binary". Monthly Notices of the Royal Astronomical Society. 480 (4): 5447–5474. arXiv: 1807.10560 . Bibcode:2018MNRAS.480.5447Z. doi: 10.1093/mnras/sty2054 . ISSN   0035-8711.
  2. 1 2 Rothermich, Austin; Faherty, Jacqueline K.; Bardalez-Gagliuffi, Daniella; Schneider, Adam C.; Kirkpatrick, J. Davy; Meisner, Aaron M.; Burgasser, Adam J.; Kuchner, Marc; Allers, Katelyn; Gagné, Jonathan; Caselden, Dan; Calamari, Emily; Popinchalk, Mark; Suárez, Genaro; Gerasimov, Roman (2024-06-01). "89 New Ultracool Dwarf Comoving Companions Identified with the Backyard Worlds: Planet 9 Citizen Science Project". The Astronomical Journal. 167 (6): 253. arXiv: 2403.04592 . Bibcode:2024AJ....167..253R. doi: 10.3847/1538-3881/ad324e . ISSN   0004-6256.
  3. ↑ Langeveld, Adam B.; Scholz, Aleks; Mužić, Koraljka; Jayawardhana, Ray; Capela, Daniel; Albert, Loïc; Doyon, René; Flagg, Laura; de Furio, Matthew (2024-08-01). "The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-Floating Planets". AJ. 168 (4): 179. arXiv: 2408.12639 . Bibcode:2024arXiv240812639L. doi: 10.3847/1538-3881/ad6f0c .
  4. 1 2 Uyama, Taichi; Currie, Thayne; Hori, Yasunori; De Rosa, Robert J.; Mede, Kyle; Brandt, Timothy D.; Kwon, Jungmi; Guyon, Olivier; Lozi, Julien; Jovanovic, Nemanja; Martinache, Frantz; Kudo, Tomoyuki; Tamura, Motohide; Kasdin, N. Jeremy; Groff, Tyler (2020-02-01). "Atmospheric Characterization and Further Orbital Modeling of κ Andromeda b". The Astronomical Journal. 159 (2): 40. arXiv: 1911.09758 . Bibcode:2020AJ....159...40U. doi: 10.3847/1538-3881/ab5afa . ISSN   0004-6256.
  5. 1 2 Kirkpatrick, J. Davy; Reid, I. Neill; Liebert, James; Cutri, Roc M.; Nelson, Brant; Beichman, Charles A.; Dahn, Conard C.; Monet, David G.; Gizis, John E.; Skrutskie, Michael F. (1999-07-01). "Dwarfs Cooler than M: The Definition of Spectral Type L Using Discoveries from the 2 Micron All-Sky Survey (2MASS)". The Astrophysical Journal. 519 (2): 802–833. Bibcode:1999ApJ...519..802K. doi:10.1086/307414. ISSN   0004-637X.
  6. ↑ Reid, I. Neill; Burgasser, A. J.; Cruz, K. L.; Kirkpatrick, J. Davy; Gizis, J. E. (2001-03-01). "Near-Infrared Spectral Classification of Late M and L Dwarfs". The Astronomical Journal. 121 (3): 1710–1721. arXiv: astro-ph/0012275 . Bibcode:2001AJ....121.1710R. doi:10.1086/319418. ISSN   0004-6256.
  7. 1 2 Burrows, Adam; Hubbard, W. B.; Lunine, J. I.; Liebert, James (2001-07-01). "The theory of brown dwarfs and extrasolar giant planets". Reviews of Modern Physics. 73 (3): 719–765. arXiv: astro-ph/0103383 . Bibcode:2001RvMP...73..719B. doi:10.1103/RevModPhys.73.719. ISSN   0034-6861.
  8. 1 2 3 Sanghi, Aniket; Liu, Michael C.; Best, William M. J.; Dupuy, Trent J.; Siverd, Robert J.; Zhang, Zhoujian; Hurt, Spencer A.; Magnier, Eugene A.; Aller, Kimberly M.; Deacon, Niall R. (2023-12-01). "The Hawaii Infrared Parallax Program. VI. The Fundamental Properties of 1000+ Ultracool Dwarfs and Planetary-mass Objects Using Optical to Mid-infrared Spectral Energy Distributions and Comparison to BT-Settl and ATMO 2020 Model Atmospheres". The Astrophysical Journal. 959 (1): 63. arXiv: 2309.03082 . Bibcode:2023ApJ...959...63S. doi: 10.3847/1538-4357/acff66 . ISSN   0004-637X.
  9. 1 2 3 Aniket, Sanghi (November 8, 2023). "Table of Ultracool Fundamental Properties". zenodo. doi:10.5281/zenodo.10086810 . Retrieved 2024-09-28.
  10. ↑ Cranmer, Steven R. (2021-09-01). "Brown Dwarfs are Violet: A New Calculation of Human-eye Colors of Main-sequence Stars and Substellar Objects". Research Notes of the American Astronomical Society. 5 (9): 201. Bibcode:2021RNAAS...5..201C. doi: 10.3847/2515-5172/ac225c . ISSN   2515-5172.
  11. ↑ Zhang, Z. H.; Pinfield, D. J.; Gálvez-Ortiz, M. C.; Burningham, B.; Lodieu, N.; Marocco, F.; Burgasser, A. J.; Day-Jones, A. C.; Allard, F.; Jones, H. R. A.; Homeier, D.; Gomes, J.; Smart, R. L. (2017-01-01). "Primeval very low-mass stars and brown dwarfs - I. Six new L subdwarfs, classification and atmospheric properties". Monthly Notices of the Royal Astronomical Society. 464 (3): 3040–3059. arXiv: 1609.07181 . Bibcode:2017MNRAS.464.3040Z. doi: 10.1093/mnras/stw2438 . ISSN   0035-8711.
  12. 1 2 Chabrier, Gilles; Baraffe, Isabelle; Phillips, Mark; Debras, Florian (2023-03-01). "Impact of a new H/He equation of state on the evolution of massive brown dwarfs. New determination of the hydrogen burning limit". Astronomy and Astrophysics. 671: A119. arXiv: 2212.07153 . Bibcode:2023A&A...671A.119C. doi:10.1051/0004-6361/202243832. ISSN   0004-6361.
  13. 1 2 Zhang, Z. H.; Homeier, D.; Pinfield, D. J.; Lodieu, N.; Jones, H. R. A.; Allard, F.; Pavlenko, Ya. V. (2017-06-01). "Primeval very low-mass stars and brown dwarfs - II. The most metal-poor substellar object". Monthly Notices of the Royal Astronomical Society. 468 (1): 261–271. arXiv: 1702.02001 . Bibcode:2017MNRAS.468..261Z. doi: 10.1093/mnras/stx350 . ISSN   0035-8711.
  14. 1 2 Burgasser, Adam J.; Gerasimov, Roman; Kremer, Kyle; Brooks, Hunter; Alvarado, Efrain; Schneider, Adam C.; Meisner, Aaron M.; Theissen, Christopher A.; Softich, Emma; Karpoor, Preethi; Bickle, Thomas P.; Kabatnik, Martin; Rothermich, Austin; Caselden, Dan; Kirkpatrick, J. Davy; Faherty, Jacqueline K; Casewell, Sarah L.; Kuchner, Marc J.; Backyard Worlds: Planet 9 Collaboration (2024-08-01). "Discovery of a Hypervelocity L Subdwarf at the Star/Brown Dwarf Mass Limit". The Astrophysical Journal. 971 (1): L25. arXiv: 2407.08578 . Bibcode:2024ApJ...971L..25B. doi: 10.3847/2041-8213/ad6607 . ISSN   0004-637X.{{cite journal}}: CS1 maint: numeric names: authors list (link)
  15. 1 2 3 4 Schneider, Adam C.; Burgasser, Adam J.; Bruursema, Justice; Munn, Jeffrey A.; Vrba, Frederick J.; Caselden, Dan; Kabatnik, Martin; Rothermich, Austin; Sainio, Arttu; Bickle, Thomas P.; Dahm, Scott E.; Meisner, Aaron M.; Kirkpatrick, J. Davy; Suárez, Genaro; Gagné, Jonathan (2023-02-01). "Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf". The Astrophysical Journal. 943 (2): L16. arXiv: 2301.02322 . Bibcode:2023ApJ...943L..16S. doi: 10.3847/2041-8213/acb0cd . ISSN   0004-637X.
  16. ↑ Luhman, K. L.; Alves de Oliveira, C.; Baraffe, I.; Chabrier, G.; Geballe, T. R.; Parker, R. J.; Pendleton, Y. J.; Tremblin, P. (January 2024). "A JWST Survey for Planetary Mass Brown Dwarfs in IC 348". The Astronomical Journal. 167 (1): 19. Bibcode:2024AJ....167...19L. doi: 10.3847/1538-3881/ad00b7 . hdl: 10871/134911 . ISSN   0004-6256.
  17. ↑ Kirkpatrick, J. Davy; Allard, France; Bida, Tom; Zuckerman, Ben; Becklin, E. E.; Chabrier, Gilles; Baraffe, Isabelle (July 1999). "An Improved Optical Spectrum and New Model FITS of the Likely Brown Dwarf GD 165B". Astrophysical Journal. 519 (2): 834–843. Bibcode:1999ApJ...519..834K. doi: 10.1086/307380 . ISSN   0004-637X.
  18. ↑ Filippazzo, Joseph C.; Rice, Emily L.; Faherty, Jacqueline; Cruz, Kelle L.; Van Gordon, Mollie M.; Looper, Dagny L. (September 2015). "Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime". Astrophysical Journal. 810 (2): 158. arXiv: 1508.01767 . Bibcode:2015ApJ...810..158F. doi:10.1088/0004-637X/810/2/158. ISSN   0004-637X. S2CID   89611607.
  19. ↑ Bailey, Vanessa; Meshkat, Tiffany; Reiter, Megan; Morzinski, Katie; Males, Jared; Su, Kate Y. L.; Hinz, Philip M.; Kenworthy, Matthew; Stark, Daniel; Mamajek, Eric; Briguglio, Runa; Close, Laird M.; Follette, Katherine B.; Puglisi, Alfio; Rodigas, Timothy (2014-01-01). "HD 106906 b: A Planetary-mass Companion Outside a Massive Debris Disk". The Astrophysical Journal. 780 (1): L4. arXiv: 1312.1265 . Bibcode:2014ApJ...780L...4B. doi:10.1088/2041-8205/780/1/L4. ISSN   0004-637X.
  20. ↑ Dupuy, Trent J.; Liu, Michael C.; Allers, Katelyn N.; Biller, Beth A.; Kratter, Kaitlin M.; Mann, Andrew W.; Shkolnik, Evgenya L.; Kraus, Adam L.; Best, William M. J. (2018-08-01). "The Hawaii Infrared Parallax Program. III. 2MASS J0249-0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group". The Astronomical Journal. 156 (2): 57. arXiv: 1807.05235 . Bibcode:2018AJ....156...57D. doi: 10.3847/1538-3881/aacbc2 . ISSN   0004-6256.
  21. ↑ Wu, Ya-Lin; Bowler, Brendan P.; Sheehan, Patrick D.; Close, Laird M.; Eisner, Joshua A.; Best, William M. J.; Ward-Duong, Kimberly; Zhu, Zhaohuan; Kraus, Adam L. (2022-05-01). "ALMA Discovery of a Disk around the Planetary-mass Companion SR 12 c". The Astrophysical Journal. 930 (1): L3. arXiv: 2204.06013 . Bibcode:2022ApJ...930L...3W. doi: 10.3847/2041-8213/ac6420 . ISSN   0004-637X.
  22. ↑ Teasdale, Matthew; Stamatellos, Dimitris (2024-09-01). "On the potential origin of the circumbinary planet Delorme 1 (AB)b". Monthly Notices of the Royal Astronomical Society. 533 (2): 2294–2302. arXiv: 2408.06231 . Bibcode:2024MNRAS.533.2294T. doi: 10.1093/mnras/stae1964 . ISSN   0035-8711.
  23. ↑ Marois, Christian; Macintosh, Bruce; Barman, Travis; Zuckerman, B.; Song, Inseok; Patience, Jennifer; Lafrenière, David; Doyon, René (2008-11-01). "Direct Imaging of Multiple Planets Orbiting the Star HR 8799". Science. 322 (5906): 1348–1352. arXiv: 0811.2606 . Bibcode:2008Sci...322.1348M. doi:10.1126/science.1166585. ISSN   0036-8075. PMID   19008415.
  24. 1 2 Luhman, K. L.; Esplin, T. L.; Loutrel, N. P. (2016-08-01). "A Census of Young Stars and Brown Dwarfs in IC 348 and NGC 1333". The Astrophysical Journal. 827 (1): 52. arXiv: 1605.08907 . Bibcode:2016ApJ...827...52L. doi: 10.3847/0004-637X/827/1/52 . ISSN   0004-637X.
  25. ↑ Cruz, Kelle L.; Kirkpatrick, J. Davy; Burgasser, Adam J. (2009-02-01). "Young L Dwarfs Identified in the Field: A Preliminary Low-Gravity, Optical Spectral Sequence from L0 to L5". The Astronomical Journal. 137 (2): 3345–3357. arXiv: 0812.0364 . Bibcode:2009AJ....137.3345C. doi:10.1088/0004-6256/137/2/3345. ISSN   0004-6256.
  26. ↑ Ackerman, Andrew S.; Marley, Mark S. (2001-08-01). "Precipitating Condensation Clouds in Substellar Atmospheres". The Astrophysical Journal. 556 (2): 872–884. arXiv: astro-ph/0103423 . Bibcode:2001ApJ...556..872A. doi:10.1086/321540. ISSN   0004-637X.
  27. ↑ Suárez, Genaro; Metchev, Stanimir (2022-07-01). "Ultracool dwarfs observed with the Spitzer infrared spectrograph - II. Emergence and sedimentation of silicate clouds in L dwarfs, and analysis of the full M5-T9 field dwarf spectroscopic sample". Monthly Notices of the Royal Astronomical Society. 513 (4): 5701–5726. arXiv: 2205.00168 . Bibcode:2022MNRAS.513.5701S. doi: 10.1093/mnras/stac1205 . ISSN   0035-8711.
  28. ↑ Vos, Johanna M.; Faherty, Jacqueline K.; Gagné, Jonathan; Marley, Mark; Metchev, Stanimir; Gizis, John; Rice, Emily L.; Cruz, Kelle (2022-01-01). "Let the Great World Spin: Revealing the Stormy, Turbulent Nature of Young Giant Exoplanet Analogs with the Spitzer Space Telescope". The Astrophysical Journal. 924 (2): 68. arXiv: 2201.04711 . Bibcode:2022ApJ...924...68V. doi: 10.3847/1538-4357/ac4502 . ISSN   0004-637X.
  29. ↑ Zhou, Yifan; Bowler, Brendan P.; Apai, Dániel; Kataria, Tiffany; Morley, Caroline V.; Bryan, Marta L.; Skemer, Andrew J.; Benneke, Björn (2022), "Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multi-epoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere", The Astronomical Journal, 164 (6): 239, arXiv: 2210.02464 , Bibcode:2022AJ....164..239Z, doi: 10.3847/1538-3881/ac9905 , S2CID   252734903
  30. ↑ Pineda, J. Sebastian; Hallinan, Gregg; Kao, Melodie M. (2017-09-01). "A Panchromatic View of Brown Dwarf Aurorae". The Astrophysical Journal. 846 (1): 75. arXiv: 1708.02942 . Bibcode:2017ApJ...846...75P. doi: 10.3847/1538-4357/aa8596 . ISSN   0004-637X.
  31. ↑ Gibbs, Aidan; Fitzgerald, Michael P. (2022-08-01). "Limits on the Auroral Generation of H+
    3     in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph"    . The Astronomical Journal. 164 (2): 63. arXiv: 2206.03595 . Bibcode:2022AJ....164...63G. doi: 10.3847/1538-3881/ac7718 . ISSN   0004-6256.
  32. ↑ Pineda, J. Sebastian; Hallinan, Gregg; Desert, Jean-Michel; Harding, Leon K. (2024-05-01). "Impact of Electron Precipitation on Brown Dwarf Atmospheres and the Missing Auroral H+
    3     Emission"    . The Astrophysical Journal. 966 (1): 58. arXiv: 2403.08852 . Bibcode:2024ApJ...966...58P. doi: 10.3847/1538-4357/ad2f9e . ISSN   0004-637X.
  33. ↑ Berger, E.; Rutledge, R. E.; Reid, I. N.; Bildsten, L.; Gizis, J. E.; Liebert, J.; Martín, E.; Basri, G.; Jayawardhana, R.; Brandeker, A.; Fleming, T. A.; Johns-Krull, C. M.; Giampapa, M. S.; Hawley, S. L.; Schmitt, J. H. M. M. (2005-07-01). "The Magnetic Properties of an L Dwarf Derived from Simultaneous Radio, X-Ray, and Hα Observations". The Astrophysical Journal. 627 (2): 960–973. arXiv: astro-ph/0502384 . Bibcode:2005ApJ...627..960B. doi:10.1086/430343. ISSN   0004-637X.
  34. ↑ Softich, Emma; Schneider, Adam C.; Patience, Jennifer; Burgasser, Adam J.; Shkolnik, Evgenya; Faherty, Jacqueline K.; Caselden, Dan; Meisner, Aaron M.; Kirkpatrick, J. Davy; Kuchner, Marc J.; Gagné, Jonathan (2022-02-01). "CWISE J014611.20-050850.0AB: The Widest Known Brown Dwarf Binary in the Field". The Astrophysical Journal. 926 (2): L12. arXiv: 2202.02315 . Bibcode:2022ApJ...926L..12S. doi: 10.3847/2041-8213/ac51d8 . ISSN   0004-637X. S2CID   246608034.
  35. ↑ Fontanive, Clémence; Biller, Beth; Bonavita, Mariangela; Allers, Katelyn (2018-09-01). "Constraining the multiplicity statistics of the coolest brown dwarfs: binary fraction continues to decrease with spectral type". Monthly Notices of the Royal Astronomical Society. 479 (2): 2702–2727. arXiv: 1806.08737 . Bibcode:2018MNRAS.479.2702F. doi: 10.1093/mnras/sty1682 . ISSN   0035-8711.
  36. ↑ Faherty, Jacqueline K.; Goodman, Sam; Caselden, Dan; Colin, Guillaume; Kuchner, Marc J.; Meisner, Aaron M.; Gagné, Jonathan; Schneider, Adam C.; Gonzales, Eileen C.; Bardalez Gagliuffi, Daniella C.; Logsdon, Sarah E.; Allers, Katelyn; Burgasser, Adam J. (2020-02-01). "WISE 2150-7520AB: A Very Low-mass, Wide Comoving Brown Dwarf System Discovered through the Citizen Science Project Backyard Worlds: Planet 9". The Astrophysical Journal. 889 (2): 176. arXiv: 1911.04600 . Bibcode:2020ApJ...889..176F. doi: 10.3847/1538-4357/ab5303 . ISSN   0004-637X.
  37. ↑ Luhman, K. L. (2013-04-01). "Discovery of a Binary Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal. 767 (1): L1. arXiv: 1303.2401 . Bibcode:2013ApJ...767L...1L. doi:10.1088/2041-8205/767/1/L1. ISSN   0004-637X.
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