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Peter Pan disk

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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

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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

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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] Two peter pan disks (J0808 and J0632) show variation due to material from the disk blocking the light of the star.[1][9] J0808 and J0501 also showed flares.[1][2] Some of the Peter Pan disks (J0446, J0949, LDS 5606 and J1915) are binaries or suspected binaries.[2][10][11] J0226 is a candidate brown dwarf[2] and Delorme 1 (AB)b is a planetary-mass object in a circumbinary orbit.[7][12][13]

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] Modelling has shown that disk can survive for 50 Myrs around stars with a mass less than 0.6 M☉ and in low-radiation environments. At higher masses of 0.6 to 0.8 M☉ the stars form an inner gap before 50 Myr, preventing accretion.[14] 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.[15] It was proposed that disks do form with a lifetime distribution, with some disks only existing for a few Myrs and others for dozens of Myrs. This would explain why some >20 Myr old M-dwarfs show accretion due to a disk, but not all M-dwarfs of this age. The research team found an initial disk fraction of 65% for M-dwarfs (M3.7-M6) and the disk lifetime distribution matches a Gaussian or Weibull distribution.[16]

Known Peter Pan disks

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Artist's Impression of a Peter Pan disk
SPHERE image of the disk around PDS 111, which is a higher-mass analogue 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.[17]

Murphy et al. found additional Peter Pan disks in the literature, which were identified as part of the Columba and Tucana-Horologium associations. The Disk Detective Collaboration identified two additional Peter Pan disks in Columba and Carina associations.[2] 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][18] 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 non-accreting.[19]

In the following years additional objects were discovered.[7][9][10][11] Some objects do not exactly fit the definition of Peter Pan disks, but are similar enough to be analogs: The object 2MASS J06195260-2903592 was found to be a 31+22
−10 Myr old analog to Peter Pan disks. This object does however not show accretion.[20] The star PDS 111 is interpreted as a higher-mass analog of Peter Pan disks, with an age of 15.9+1.7
−3.7 Myrs, a mass of 1.2±0.1 M☉, active accretion and a directly imaged disk.[21] One team also found old accreting stars in the Large Magellanic Cloud in the Tarantula Nebula.[22] This might be explained with a low metallicity in the LMC, which can lead to more massive disks that are less opaque.[14]

List of Peter Pan disk candidates

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Name Age (Myrs) Association spectral type infrared excess accretion Reference
WISE J080822.18-644357.3 45+11
−7 		Carina association M5 yes yes [3][4]
2MASS J05010082-4337102 42+6
−4 		Columba association M4.5 yes yes [2][23]
2MASS J02265658-5327032 45±4 Tucana-Horologium association L0δ yes yes [2][23]
WISEA J044634.16-262756.1 42+6
−4 		Columba association (but might be χ1 Fornacis member, which is 34 Myr old) M6+M6 yes likely [2][24]
WISEA J094900.65-713803.1 45+11
−7 		Carina association M4+M5 yes yes both [2]
2MASS J15460752-6258042 ~55 Argus association (but might be Beta Pictoris member) M5 yes yes [10][24]
2MASS J05082729−2101444 30-44 Columba association (but could be Beta Pictoris member) M5 yes yes [10]
LDS 5606 30-44 Columba association (but could be Beta Pictoris member) M5+M5 yes yes [25][10]
Delorme 1 (AB)b 30-45 Tucana-Horologium association L0 (very low gravity) no yes [7][12][13]
2MASS J06320799-6810419 ~45 Carina association M4.5 yes yes [9]
2MASS J19150079-2847587 24±3 Beta Pictoris moving group M4.8 (binary candidate) yes yes [11]
StHα34 24.7+0.9
−0.6 		Beta Pictoris moving group M3+M3 yes yes [24][26][27]

2MASS J0041353-562112 was discarded as it belongs to the Beta Pictoris moving group and does not show excess.[2]

Implications for planet formation around M-stars

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There are different models to explain the existence of Peter Pan disks, such as disrupted planetesimals[4] or recent collisions of planetary bodies.[28] 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.[9]

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.[29]

See also

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References

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  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 o p q r 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. ^ a b 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 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. ^ a b c d 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. ^ a b c d 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 (1): 1386–1402. arXiv:2204.14163. Bibcode:2022MNRAS.514.1386G. doi:10.1093/mnras/stac1433. ISSN 0035-8711.
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  11. ^ a b c Stahl, Asa G.; Johns-Krull, Christopher M.; Flagg, L. (2022-12-01). "Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups". The Astrophysical Journal. 941 (1): 101. Bibcode:2022ApJ...941..101S. doi:10.3847/1538-4357/ac8b78. ISSN 0004-637X.
  12. ^ a b Betti, S. K.; Follette, K. B.; Ward-Duong, K.; Aoyama, Y.; Marleau, G. -D.; Bary, J.; Robinson, C.; Janson, M.; Balmer, W.; Chauvin, G.; Palma-Bifani, P. (2022-08-01). "Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b". The Astrophysical Journal. 935 (1): L18. arXiv:2208.05016. Bibcode:2022ApJ...935L..18B. doi:10.3847/2041-8213/ac85ef. ISSN 0004-637X.
  13. ^ a b Ringqvist, Simon C.; Viswanath, Gayathri; Aoyama, Yuhiko; Janson, Markus; Marleau, Gabriel-Dominique; Brandeker, Alexis (2023-01-01). "Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b. Indications of magnetospheric accretion". Astronomy and Astrophysics. 669: L12. arXiv:2212.03207. Bibcode:2023A&A...669L..12R. doi:10.1051/0004-6361/202245424. ISSN 0004-6361.
  14. ^ a b Wilhelm, Martijn J. C.; Portegies Zwart, Simon (2022-01-01). "Exploring the possibility of Peter Pan discs across stellar mass". Monthly Notices of the Royal Astronomical Society. 509 (1): 44–51. arXiv:2109.01456. Bibcode:2022MNRAS.509...44W. doi:10.1093/mnras/stab2523. ISSN 0035-8711.
  15. ^ 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.
  16. ^ Pfalzner, Susanne; Dincer, Furkan (2024-03-01). "Low-mass Stars: Their Protoplanetary Disk Lifetime Distribution". The Astrophysical Journal. 963 (2): 122. arXiv:2401.03775. Bibcode:2024ApJ...963..122P. doi:10.3847/1538-4357/ad1bef. ISSN 0004-637X.
  17. ^ Ramsey, Sarah (2016-10-21). "Citizen Scientists Discover Potential New Exoplanet Hunting Ground". NASA. Retrieved 2020-01-22.
  18. ^ 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.
  19. ^ 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.
  20. ^ Liu, Michael C.; Magnier, Eugene A.; Zhang, Zhoujian; Gaidos, Eric; Dupuy, Trent J.; Liu, Pengyu; Biller, Beth A.; Vos, Johanna M.; Allers, Katelyn N.; Hinkle, Jason T.; Shappee, Benjamin J.; Constantinou, Sage N. L.; Dennis, Mitchell T.; Emerson, Kenji S. (2022-10-01). "On the Unusual Variability of 2MASS J06195260-2903592: A Long-lived Disk around a Young Ultracool Dwarf". The Astronomical Journal. 164 (4): 165. arXiv:2208.14551. Bibcode:2022AJ....164..165L. doi:10.3847/1538-3881/ac8cee. ISSN 0004-6256.
  21. ^ Derkink, Annelotte; Ginski, Christian; Pinilla, Paola; Kurtovic, Nicolas; Kaper, Lex; de Koter, Alex; Valegård, Per-Gunnar; Mamajek, Eric; Backs, Frank; Benisty, Myriam; Birnstiel, Til; Columba, Gabriele; Dominik, Carsten; Garufi, Antonio; Hogerheijde, Michiel (2024-08-01). "Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): PDS 111, an old T Tauri star with a young-looking disk". Astronomy and Astrophysics. 688: A149. arXiv:2406.04160. Bibcode:2024A&A...688A.149D. doi:10.1051/0004-6361/202348555. ISSN 0004-6361.
  22. ^ De Marchi, Guido; Panagia, Nino; Beccari, Giacomo (2017-09-01). "Photometric Determination of the Mass Accretion Rates of Pre-main-sequence Stars. V. Recent Star Formation in the 30 Dor Nebula". The Astrophysical Journal. 846 (2): 110. arXiv:1708.03631. Bibcode:2017ApJ...846..110D. doi:10.3847/1538-4357/aa85e9. ISSN 0004-637X.
  23. ^ a b 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.
  24. ^ a b c Luhman, K. L. (2024-10-01). "A Census of the β Pic Moving Group and Other Nearby Associations with Gaia". The Astronomical Journal. 168 (4): 159. arXiv:2409.06092. Bibcode:2024AJ....168..159L. doi:10.3847/1538-3881/ad697d. ISSN 0004-6256.
  25. ^ Rodriguez, David R.; Zuckerman, Ben; Faherty, Jacqueline K.; Vican, Laura (2014-07-01). "A dusty M5 binary in the β Pictoris moving group". Astronomy and Astrophysics. 567: A20. arXiv:1404.2543. Bibcode:2014A&A...567A..20R. doi:10.1051/0004-6361/201423604. ISSN 0004-6361.
  26. ^ White, Russel J.; Hillenbrand, Lynne A. (2005-03-01). "A Long-lived Accretion Disk around a Lithium-depleted Binary T Tauri Star". The Astrophysical Journal. 621 (1): L65–L68. arXiv:astro-ph/0501307. Bibcode:2005ApJ...621L..65W. doi:10.1086/428752. ISSN 0004-637X.
  27. ^ Hartmann, Lee; Calvet, Nuria; Watson, Dan M.; D'Alessio, P.; Furlan, E.; Sargent, B.; Forrest, W. J.; Uchida, K. I.; Green, J. D.; Sloan, G. C.; Chen, C. H.; Najita, J.; Kemper, F.; Herter, T. L.; Morris, P. (2005-08-01). "The Accretion Disk of the Lithium-depleted Young Binary St 34". The Astrophysical Journal. 628 (2): L147–L150. Bibcode:2005ApJ...628L.147H. doi:10.1086/432756. ISSN 0004-637X.
  28. ^ 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.
  29. ^ 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. arXiv:2209.11160. Bibcode:2023AJ....165..120K. doi:10.3847/1538-3881/acabce. hdl:20.500.11850/601567. ISSN 0004-6256.
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