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Peter Pan disk

January 01, 1970

A Peter Pan disk is a circumstellar disk around a star or brown dwarf that appears to have retained enough gas to form a gas giant planet for much longer than the typically assumed gas dispersal timescale of approximately 5 million years. Several examples of such disks have been observed to orbit stars with spectral types of M or later. The presence of gas around these disks has generally been inferred from the total amount of radiation emitted from the disk at infrared wavelengths, and/or spectroscopic signatures of hydrogen accreting onto the star. To fit one specific definition of a Peter Pan disk, the source needs to have an infrared "color" of , an age of >20 Myr and spectroscopic evidence of accretion.[1][2]

In 2016 volunteers of the Disk Detective project discovered WISE J080822.18-644357.3 (or J0808). This low-mass star showed signs of youth, for example a strong infrared excess and active accretion of gaseous material. It is part of the 45+11
−7 Myr old Carina young moving group, older than expected for these characteristics of an M-dwarf.[3][4] Other stars and brown dwarfs were discovered to be similar to J0808, with signs of youth while being in an older moving group.[4][2] Together with J0808, these older low-mass accretors in nearby moving groups have been called Peter Pan disks in one scientific paper published in early 2020.[5][2] Since then the term was used by other independent research groups.[6][7][8]

Name edit

Peter Pan disks are named after the main character Peter Pan in the play and book Peter Pan, or The Boy Who Wouldn’t Grow Up, written by J.M. Barrie in 1904. The Peter Pan disks have a young appearance, while being old in years. In other words: The Peter Pan disks "refuse to grow up", a feature they share with the lost boys and titular character in Peter Pan.[2][1]

Characteristics edit

The known Peter Pan disks have the H-alpha spectroscopic line as a sign of accretion. J0808 shows variations in the Paschen-β and Brackett-γ lines, which is a clear sign of accretion.[1][2] It was also identified as lithium-rich, which is a sign of youth.[4]

It was suggested that Peter Pan disks take longer to dissipate due to lower photoevaporation caused by lower far-ultraviolet and X-ray emission coming from the M-dwarf.[2] Observations with the Chandra X-ray Observatory showed that Peter Pan Disks have a similar X-ray luminosity as field M-dwarfs, with properties similar to weak-lined T Tauri stars. The researchers of this study concluded that the current X-ray luminosity of Peter Pan disk cannot explain their old age. The old age of the disk could be the result of weaker far-ultraviolet flux incident on the disk, due to weaker accretion in the pre-main sequence stage.[9]

J0808 shows variations in the light curve from CTIO, which could be disk material blocking light from the star. The source also showed a strong flare.[1][2] It shows three distinct disk components: A "hot" inner disk with a temperature of 1100 K (827 °C or 1520 °F), located at 0.0056 au. A "warm" outer disk with a temperature of 240 K (-33 °C or -28 °F), located at 0.115 au.[4] A "cold" outer disk with a temperature of 20 K (-253 °C or -424 °F), located at <16 au.[10]

2MASS J05010082-4337102 showed a flare in a TESS light curve and periodic variations, which could be due to starspots. The system is inclined to our line of sight by ~38°, enough to not expect any disk material to move in front of the star.[1][2]

WISEA J044634.16-262756.1 and WISEA J094900.65-713803.1 are both apparent visual double in Gaia data.[2]

2MASS J02265658-5327032 is a candidate brown dwarf with a Peter Pan disk.[2]

2M0632 was observed by TESS and it shows variability due to material from the disk transiting in front of the star.[11]

Known Peter Pan disks edit

 
Artist's Impression of a Peter Pan disk

The prototype Peter Pan disk is WISE J080822.18-644357.3.[2] It was discovered by the NASA-led citizen science project Disk Detective.[12]

Murphy et al. found additional Peter Pan disks in the literature, which were identified as part of the Columba and Tucana-Horologium associations.[13][4] Examples are 2MASS J0041353-562112 in Tuc-Hor,[14][15] 2MASS J05010082-4337102 in Columba and 2MASS J02265658-5327032 in Tuc-Hor.[16] The Tuc-Hor association has an age of 45±4 Myr and the Columba association has an age of 42+6
−4 Myr. 2MASS J0041353-562112 was later discarded as it does not show excess and could belong to the Beta Pictoris moving group.[2]

The Disk Detective Collaboration identified two additional Peter Pan disks: WISEAJ044634.16-262756.1 in Columba and WISEA J094900.65-713803.1 in Carina. Both systems are visual doubles. The paper also mentions that members of NGC 2547 were previously identified to have 22 μm excess and could be similar to Peter Pan disks.[2][17] 2MASS 08093547-4913033, which is one of the M-dwarfs with a debris disk in NGC 2547 was observed with the Spitzer Infrared Spectrograph. In this system the first detection of silicate was made from a debris disk around an M-type star. While the system shows the H-alpha line, it was interpreted to be devoid of gas and nonaccreting.[18]

Implications for planet formation around M-stars edit

There are different models to explain the existence of Peter Pan disks, such as disrupted planetesimals[4] or recent collisions of planetary bodies.[10] One explanation is that Peter Pan disks are long-lived primordial disks.[6] This would follow the trend of lower-mass stars requiring more time to dissipate their disks. Exoplanets around M-stars would have more time to form, significantly affecting the atmospheres on these planets.[1][2]

Peter Pan disks that form multiplanetary systems could force the planets in close-in, resonant orbits. The 7-planet system TRAPPIST-1 could be an end result of such a Peter Pan disk.[11]

A Peter Pan disk could also help to explain the existence of Jovian planets around M-dwarfs, such as TOI-5205b. A longer lifetime for a disk would give more time for a solid core to form, which could initiate runaway core-accretion.[19]

See also edit

References edit

  1. ^ a b c d e f silverbergastro (2020-01-17). "Our New Paper: "Peter Pan Disks"!". Disk Detective. Retrieved 2020-01-22.
  2. ^ a b c d e f g h i j k l m n Silverberg, Steven M.; Wisniewski, John P.; Kuchner, Marc J.; Lawson, Kellen D.; Bans, Alissa S.; Debes, John H.; Biggs, Joseph R.; Bosch, Milton K. D.; Doll, Katharina; Luca, Hugo A. Durantini; Enachioaie, Alexandru; Hamilton, Joshua; Holden, Jonathan; Hyogo, Michiharu; the Disk Detective Collaboration (2020-01-14). "Peter Pan Disks: Long-lived Accretion Disks Around Young M Stars". The Astrophysical Journal. 890 (2): 106. arXiv:2001.05030. Bibcode:2020ApJ...890..106S. doi:10.3847/1538-4357/ab68e6. S2CID 210718358.
  3. ^ Silverberg, Steven M.; Kuchner, Marc J.; Wisniewski, John P.; Gagné, Jonathan; Bans, Alissa S.; Bhattacharjee, Shambo; Currie, Thayne R.; Debes, John R.; Biggs, Joseph R. (14 October 2016). "A New M Dwarf Debris Disk Candidate in a Young Moving Group Discovered with Disk Detective". The Astrophysical Journal. 830 (2): L28. arXiv:1610.05293. Bibcode:2016ApJ...830L..28S. doi:10.3847/2041-8205/830/2/L28. ISSN 2041-8205. S2CID 119183849.
  4. ^ a b c d e f Murphy, Simon J.; Mamajek, Eric E.; Bell, Cameron P. M. (2018-05-21). "WISE J080822.18−644357.3 – a 45 Myr-old accreting M dwarf hosting a primordial disc". Monthly Notices of the Royal Astronomical Society. 476 (3): 3290–3302. arXiv:1703.04544. Bibcode:2018MNRAS.476.3290M. doi:10.1093/mnras/sty471. ISSN 0035-8711. S2CID 119341475.
  5. ^ "Low-mass Stars | Steven M. Silverberg". www.nhn.ou.edu. Retrieved 2019-07-25.
  6. ^ a b Coleman, Gavin; Haworth, Thomas J. (June 2020). "Peter Pan discs: finding Neverland's parameters". Monthly Notices of the Royal Astronomical Society. 496 (1): 111. arXiv:2006.06115. Bibcode:2020MNRAS.496L.111C. doi:10.1093/mnrasl/slaa098. S2CID 219573224.
  7. ^ Eriksson, Simon C.; Asensio Torres, Rubén; Janson, Markus; Aoyama, Yuhiko; Marleau, Gabriel-Dominique; Bonnefoy, Mickael; Petrus, Simon (2020-06-01). "Strong Halpha emission and signs of accretion in a circumbinary planetary mass companion from MUSE". Astronomy and Astrophysics. 638: L6. arXiv:2005.11725. Bibcode:2020A&A...638L...6E. doi:10.1051/0004-6361/202038131. ISSN 0004-6361. S2CID 218870278.
  8. ^ Dai, Fei; Winn, Joshua N.; Schlaufman, Kevin; Wang, Songhu; Weiss, Lauren; Petigura, Erik A.; Howard, Andrew W.; Fang, Min (2020-06-01). "California-Kepler Survey. IX. Revisiting the Minimum-mass Extrasolar Nebula with Precise Stellar Parameters". The Astronomical Journal. 159 (6): 247. arXiv:2004.04847. Bibcode:2020AJ....159..247D. doi:10.3847/1538-3881/ab88b8. S2CID 215736954.
  9. ^ Laos, Stefan; Wisniewski, John P.; Kuchner, Marc J.; Silverberg, Steven M.; Günther, Hans Moritz; Principe, David A.; Bonine, Brett; Kounkel, Marina; The Disk Detective Collaboration (2022-08-01). "Chandra Observations of Six Peter Pan Disks: Diversity of X-Ray-driven Internal Photoevaporation Rates Does Not Explain Their Rare Longevity". The Astrophysical Journal. 935 (2): 111. arXiv:2207.07140. Bibcode:2022ApJ...935..111L. doi:10.3847/1538-4357/ac8156. ISSN 0004-637X.
  10. ^ a b Flaherty, Kevin M.; Hughes, A. Meredith; Mamajek, Eric E.; Murphy, Simon J. (2019-02-13). "The Planet Formation Potential Around a 45 Myr old Accreting M Dwarf". The Astrophysical Journal. 872 (1): 92. arXiv:1812.04124. Bibcode:2019ApJ...872...92F. doi:10.3847/1538-4357/aaf794. ISSN 1538-4357. S2CID 119251811.
  11. ^ a b Gaidos, Eric; Mann, Andrew W.; Rojas-Ayala, Bárbara; Feiden, Gregory A.; Wood, Mackenna L.; Narayanan, Suchitra; Ansdell, Megan; Jacobs, Tom; LaCourse, Daryll (2022-07-01). "Planetesimals around stars with TESS (PAST) - II. An M dwarf 'dipper' star with a long-lived disc in the TESS continuous viewing zone". Monthly Notices of the Royal Astronomical Society. 514: 1386–1402. arXiv:2204.14163. Bibcode:2022MNRAS.514.1386G. doi:10.1093/mnras/stac1433. ISSN 0035-8711.
  12. ^ Ramsey, Sarah (2016-10-21). "Citizen Scientists Discover Potential New Exoplanet Hunting Ground". NASA. Retrieved 2020-01-22.
  13. ^ Torres, C.A.O.; Quast, G.R.; Melo, C.H.F.; Sterzik, M.F. (2008). "Young Nearby Loose Associations - aspmonographs.org". arXiv:0808.3362 [astro-ph].
  14. ^ Reiners, Ansgar (21 August 2009). "Evidence for Accretion in a Nearby, Young Brown Dwarf". The Astrophysical Journal. 702 (2): L119–L123. arXiv:0908.3482. Bibcode:2009ApJ...702L.119R. doi:10.1088/0004-637X/702/2/L119. ISSN 1538-4357. S2CID 16903320.
  15. ^ Gagné, Jonathan; Lafrenière, David; Doyon, René; Malo, Lison; Artigau, Étienne (24 February 2014). "Banyan. Ii. Very Low Mass and Substellar Candidate Members to Nearby, Young Kinematic Groups with Previously Known Signs of Youth". The Astrophysical Journal. 783 (2): 121. arXiv:1312.5864. Bibcode:2014ApJ...783..121G. doi:10.1088/0004-637X/783/2/121. ISSN 0004-637X. S2CID 119251619.
  16. ^ Boucher, Anne; Lafrenière, David; Gagné, Jonathan; Malo, Lison; Faherty, Jacqueline K.; Doyon, René; Chen, Christine H. (15 November 2016). "Banyan. Viii. New Low-Mass Stars and Brown Dwarfs with Candidate Circumstellar Disks". The Astrophysical Journal. 832 (1): 50. arXiv:1608.08259. Bibcode:2016ApJ...832...50B. doi:10.3847/0004-637X/832/1/50. ISSN 0004-637X. S2CID 119017727.
  17. ^ Forbrich, Jan; Lada, Charles J.; Muench, August A.; Teixeira, Paula S. (November 2008). "New M Dwarf Debris Disk Candidates in NGC 2547". The Astrophysical Journal. 687 (2): 1107. arXiv:0807.3597. Bibcode:2008ApJ...687.1107F. doi:10.1086/592035. ISSN 0004-637X. S2CID 119215678.
  18. ^ Teixeira, Paula S.; Lada, Charles J.; Wood, Kenneth; Robitaille, Thomas P.; Luhman, Kevin L. (July 2009). "Infrared Spectrograph Characterization of a Debris Disk Around an M-Type Star in NGC 2547". The Astrophysical Journal. 700 (1): 454–459. arXiv:0905.2469. Bibcode:2009ApJ...700..454T. doi:10.1088/0004-637X/700/1/454. ISSN 0004-637X. S2CID 8231130.
  19. ^ Kanodia, Shubham; Mahadevan, Suvrath; Libby-Roberts, Jessica; Stefansson, Gudmundur; Cañas, Caleb I.; Piette, Anjali A. A.; Boss, Alan; Teske, Johanna; Chambers, John; Zeimann, Greg; Monson, Andrew; Robertson, Paul; Ninan, Joe P.; Lin, Andrea S. J.; Bender, Chad F. (2023-03-01). "TOI-5205b: A Short-period Jovian Planet Transiting a Mid-M Dwarf". The Astronomical Journal. 165 (3): 120. Bibcode:2023AJ....165..120K. doi:10.3847/1538-3881/acabce. hdl:20.500.11850/601567. ISSN 0004-6256.

External links edit

  • AWI0005x3s talk page at diskdetective.org
  • NASA Citizen Scientists Discover “Peter Pan Disks”

January 01, 1970
peter, disk, circumstellar, disk, around, star, brown, dwarf, that, appears, have, retained, enough, form, giant, planet, much, longer, than, typically, assumed, dispersal, timescale, approximately, million, years, several, examples, such, disks, have, been, o. A Peter Pan disk is a circumstellar disk around a star or brown dwarf that appears to have retained enough gas to form a gas giant planet for much longer than the typically assumed gas dispersal timescale of approximately 5 million years Several examples of such disks have been observed to orbit stars with spectral types of M or later The presence of gas around these disks has generally been inferred from the total amount of radiation emitted from the disk at infrared wavelengths and or spectroscopic signatures of hydrogen accreting onto the star To fit one specific definition of a Peter Pan disk the source needs to have an infrared color of K s W 4 gt 2 displaystyle Ks W4 gt 2 an age of gt 20 Myr and spectroscopic evidence of accretion 1 2 In 2016 volunteers of the Disk Detective project discovered WISE J080822 18 644357 3 or J0808 This low mass star showed signs of youth for example a strong infrared excess and active accretion of gaseous material It is part of the 45 11 7 Myr old Carina young moving group older than expected for these characteristics of an M dwarf 3 4 Other stars and brown dwarfs were discovered to be similar to J0808 with signs of youth while being in an older moving group 4 2 Together with J0808 these older low mass accretors in nearby moving groups have been called Peter Pan disks in one scientific paper published in early 2020 5 2 Since then the term was used by other independent research groups 6 7 8 Contents 1 Name 2 Characteristics 3 Known Peter Pan disks 4 Implications for planet formation around M stars 5 See also 6 References 7 External linksName editPeter Pan disks are named after the main character Peter Pan in the play and book Peter Pan or The Boy Who Wouldn t Grow Up written by J M Barrie in 1904 The Peter Pan disks have a young appearance while being old in years In other words The Peter Pan disks refuse to grow up a feature they share with the lost boys and titular character in Peter Pan 2 1 Characteristics editThe known Peter Pan disks have the H alpha spectroscopic line as a sign of accretion J0808 shows variations in the Paschen b and Brackett g lines which is a clear sign of accretion 1 2 It was also identified as lithium rich which is a sign of youth 4 It was suggested that Peter Pan disks take longer to dissipate due to lower photoevaporation caused by lower far ultraviolet and X ray emission coming from the M dwarf 2 Observations with the Chandra X ray Observatory showed that Peter Pan Disks have a similar X ray luminosity as field M dwarfs with properties similar to weak lined T Tauri stars The researchers of this study concluded that the current X ray luminosity of Peter Pan disk cannot explain their old age The old age of the disk could be the result of weaker far ultraviolet flux incident on the disk due to weaker accretion in the pre main sequence stage 9 J0808 shows variations in the light curve from CTIO which could be disk material blocking light from the star The source also showed a strong flare 1 2 It shows three distinct disk components A hot inner disk with a temperature of 1100 K 827 C or 1520 F located at 0 0056 au A warm outer disk with a temperature of 240 K 33 C or 28 F located at 0 115 au 4 A cold outer disk with a temperature of 20 K 253 C or 424 F located at lt 16 au 10 2MASS J05010082 4337102 showed a flare in a TESS light curve and periodic variations which could be due to starspots The system is inclined to our line of sight by 38 enough to not expect any disk material to move in front of the star 1 2 WISEA J044634 16 262756 1 and WISEA J094900 65 713803 1 are both apparent visual double in Gaia data 2 2MASS J02265658 5327032 is a candidate brown dwarf with a Peter Pan disk 2 2M0632 was observed by TESS and it shows variability due to material from the disk transiting in front of the star 11 Known Peter Pan disks edit nbsp Artist s Impression of a Peter Pan disk The prototype Peter Pan disk is WISE J080822 18 644357 3 2 It was discovered by the NASA led citizen science project Disk Detective 12 Murphy et al found additional Peter Pan disks in the literature which were identified as part of the Columba and Tucana Horologium associations 13 4 Examples are 2MASS J0041353 562112 in Tuc Hor 14 15 2MASS J05010082 4337102 in Columba and 2MASS J02265658 5327032 in Tuc Hor 16 The Tuc Hor association has an age of 45 4 Myr and the Columba association has an age of 42 6 4 Myr 2MASS J0041353 562112 was later discarded as it does not show excess and could belong to the Beta Pictoris moving group 2 The Disk Detective Collaboration identified two additional Peter Pan disks WISEAJ044634 16 262756 1 in Columba and WISEA J094900 65 713803 1 in Carina Both systems are visual doubles The paper also mentions that members of NGC 2547 were previously identified to have 22 mm excess and could be similar to Peter Pan disks 2 17 2MASS 08093547 4913033 which is one of the M dwarfs with a debris disk in NGC 2547 was observed with the Spitzer Infrared Spectrograph In this system the first detection of silicate was made from a debris disk around an M type star While the system shows the H alpha line it was interpreted to be devoid of gas and nonaccreting 18 Implications for planet formation around M stars editThere are different models to explain the existence of Peter Pan disks such as disrupted planetesimals 4 or recent collisions of planetary bodies 10 One explanation is that Peter Pan disks are long lived primordial disks 6 This would follow the trend of lower mass stars requiring more time to dissipate their disks Exoplanets around M stars would have more time to form significantly affecting the atmospheres on these planets 1 2 Peter Pan disks that form multiplanetary systems could force the planets in close in resonant orbits The 7 planet system TRAPPIST 1 could be an end result of such a Peter Pan disk 11 A Peter Pan disk could also help to explain the existence of Jovian planets around M dwarfs such as TOI 5205b A longer lifetime for a disk would give more time for a solid core to form which could initiate runaway core accretion 19 See also editWISE J080822 18 644357 3 Disk Detective Circumstellar disk Protoplanetary disk Debris disk T Tauri star HD 74389 AU MicroscopiiReferences edit a b c d e f silverbergastro 2020 01 17 Our New Paper Peter Pan Disks Disk Detective Retrieved 2020 01 22 a b c d e f g h i j k l m n Silverberg Steven M Wisniewski John P Kuchner Marc J Lawson Kellen D Bans Alissa S Debes John H Biggs Joseph R Bosch Milton K D Doll Katharina Luca Hugo A Durantini Enachioaie Alexandru Hamilton Joshua Holden Jonathan Hyogo Michiharu the Disk Detective Collaboration 2020 01 14 Peter Pan Disks Long lived Accretion Disks Around Young M Stars The Astrophysical Journal 890 2 106 arXiv 2001 05030 Bibcode 2020ApJ 890 106S doi 10 3847 1538 4357 ab68e6 S2CID 210718358 Silverberg Steven M Kuchner Marc J Wisniewski John P Gagne Jonathan Bans Alissa S Bhattacharjee Shambo Currie Thayne R Debes John R Biggs Joseph R 14 October 2016 A New M Dwarf Debris Disk Candidate in a Young Moving Group Discovered with Disk Detective The Astrophysical Journal 830 2 L28 arXiv 1610 05293 Bibcode 2016ApJ 830L 28S doi 10 3847 2041 8205 830 2 L28 ISSN 2041 8205 S2CID 119183849 a b c d e f Murphy Simon J Mamajek Eric E Bell Cameron P M 2018 05 21 WISE J080822 18 644357 3 a 45 Myr old accreting M dwarf hosting a primordial disc Monthly Notices of the Royal Astronomical Society 476 3 3290 3302 arXiv 1703 04544 Bibcode 2018MNRAS 476 3290M doi 10 1093 mnras sty471 ISSN 0035 8711 S2CID 119341475 Low mass Stars Steven M Silverberg www nhn ou edu Retrieved 2019 07 25 a b Coleman Gavin Haworth Thomas J June 2020 Peter Pan discs finding Neverland s parameters Monthly Notices of the Royal Astronomical Society 496 1 111 arXiv 2006 06115 Bibcode 2020MNRAS 496L 111C doi 10 1093 mnrasl slaa098 S2CID 219573224 Eriksson Simon C Asensio Torres Ruben Janson Markus Aoyama Yuhiko Marleau Gabriel Dominique Bonnefoy Mickael Petrus Simon 2020 06 01 Strong Halpha emission and signs of accretion in a circumbinary planetary mass companion from MUSE Astronomy and Astrophysics 638 L6 arXiv 2005 11725 Bibcode 2020A amp A 638L 6E doi 10 1051 0004 6361 202038131 ISSN 0004 6361 S2CID 218870278 Dai Fei Winn Joshua N Schlaufman Kevin Wang Songhu Weiss Lauren Petigura Erik A Howard Andrew W Fang Min 2020 06 01 California Kepler Survey IX Revisiting the Minimum mass Extrasolar Nebula with Precise Stellar Parameters The Astronomical Journal 159 6 247 arXiv 2004 04847 Bibcode 2020AJ 159 247D doi 10 3847 1538 3881 ab88b8 S2CID 215736954 Laos Stefan Wisniewski John P Kuchner Marc J Silverberg Steven M Gunther Hans Moritz Principe David A Bonine Brett Kounkel Marina The Disk Detective Collaboration 2022 08 01 Chandra Observations of Six Peter Pan Disks Diversity of X Ray driven Internal Photoevaporation Rates Does Not Explain Their Rare Longevity The Astrophysical Journal 935 2 111 arXiv 2207 07140 Bibcode 2022ApJ 935 111L doi 10 3847 1538 4357 ac8156 ISSN 0004 637X a b Flaherty Kevin M Hughes A Meredith Mamajek Eric E Murphy Simon J 2019 02 13 The Planet Formation Potential Around a 45 Myr old Accreting M Dwarf The Astrophysical Journal 872 1 92 arXiv 1812 04124 Bibcode 2019ApJ 872 92F doi 10 3847 1538 4357 aaf794 ISSN 1538 4357 S2CID 119251811 a b Gaidos Eric Mann Andrew W Rojas Ayala Barbara Feiden Gregory A Wood Mackenna L Narayanan Suchitra Ansdell Megan Jacobs Tom LaCourse Daryll 2022 07 01 Planetesimals around stars with TESS PAST II An M dwarf dipper star with a long lived disc in the TESS continuous viewing zone Monthly Notices of the Royal Astronomical Society 514 1386 1402 arXiv 2204 14163 Bibcode 2022MNRAS 514 1386G doi 10 1093 mnras stac1433 ISSN 0035 8711 Ramsey Sarah 2016 10 21 Citizen Scientists Discover Potential New Exoplanet Hunting Ground NASA Retrieved 2020 01 22 Torres C A O Quast G R Melo C H F Sterzik M F 2008 Young Nearby Loose Associations aspmonographs org arXiv 0808 3362 astro ph Reiners Ansgar 21 August 2009 Evidence for Accretion in a Nearby Young Brown Dwarf The Astrophysical Journal 702 2 L119 L123 arXiv 0908 3482 Bibcode 2009ApJ 702L 119R doi 10 1088 0004 637X 702 2 L119 ISSN 1538 4357 S2CID 16903320 Gagne Jonathan Lafreniere David Doyon Rene Malo Lison Artigau Etienne 24 February 2014 Banyan Ii Very Low Mass and Substellar Candidate Members to Nearby Young Kinematic Groups with Previously Known Signs of Youth The Astrophysical Journal 783 2 121 arXiv 1312 5864 Bibcode 2014ApJ 783 121G doi 10 1088 0004 637X 783 2 121 ISSN 0004 637X S2CID 119251619 Boucher Anne Lafreniere David Gagne Jonathan Malo Lison Faherty Jacqueline K Doyon Rene Chen Christine H 15 November 2016 Banyan Viii New Low Mass Stars and Brown Dwarfs with Candidate Circumstellar Disks The Astrophysical Journal 832 1 50 arXiv 1608 08259 Bibcode 2016ApJ 832 50B doi 10 3847 0004 637X 832 1 50 ISSN 0004 637X S2CID 119017727 Forbrich Jan Lada Charles J Muench August A Teixeira Paula S November 2008 New M Dwarf Debris Disk Candidates in NGC 2547 The Astrophysical Journal 687 2 1107 arXiv 0807 3597 Bibcode 2008ApJ 687 1107F doi 10 1086 592035 ISSN 0004 637X S2CID 119215678 Teixeira Paula S Lada Charles J Wood Kenneth Robitaille Thomas P Luhman Kevin L July 2009 Infrared Spectrograph Characterization of a Debris Disk Around an M Type Star in NGC 2547 The Astrophysical Journal 700 1 454 459 arXiv 0905 2469 Bibcode 2009ApJ 700 454T doi 10 1088 0004 637X 700 1 454 ISSN 0004 637X S2CID 8231130 Kanodia Shubham Mahadevan Suvrath Libby Roberts Jessica Stefansson Gudmundur Canas Caleb I Piette Anjali A A Boss Alan Teske Johanna Chambers John Zeimann Greg Monson Andrew Robertson Paul Ninan Joe P Lin Andrea S J Bender Chad F 2023 03 01 TOI 5205b A Short period Jovian Planet Transiting a Mid M Dwarf The Astronomical Journal 165 3 120 Bibcode 2023AJ 165 120K doi 10 3847 1538 3881 acabce hdl 20 500 11850 601567 ISSN 0004 6256 External links editAWI0005x3s talk page at diskdetective org NASA Citizen Scientists Discover Peter Pan Disks Retrieved from https en wikipedia org w index php title Peter Pan disk amp oldid 1193486025, wikipedia, wiki, book, books, library,

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