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]

Contents

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

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

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

Artist's Impression of a Peter Pan disk Peter Pan disk.png
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

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

Related Research Articles

<span class="mw-page-title-main">Brown dwarf</span> Type of substellar object larger than a planet

Brown dwarfs are substellar objects that have more mass than the biggest gas giant planets, but less than the least massive main-sequence stars. Their mass is approximately 13 to 80 times that of Jupiter (MJ) -- not big enough to sustain nuclear fusion of ordinary hydrogen (1H) into helium in their cores, but massive enough to emit some light and heat from the fusion of deuterium (2H). The most massive ones can burn lithium (7Li).

<span class="mw-page-title-main">Rogue planet</span> Planetary objects without a planetary system

A rogueplanet, also termed a free-floating planet (FFP) or an isolated planetary-mass object (iPMO), is an interstellar object of planetary mass which is not gravitationally bound to any star or brown dwarf.

<span class="mw-page-title-main">NGC 2547</span> Open cluster in the constellation Vela

NGC 2547 is a southern open cluster in Vela, discovered by Nicolas Louis de Lacaille in 1751 from South Africa. The star cluster is young with an age of 20-30 million years.

2MASS J05325346+8246465 is possibly the first brown dwarf observed in the galactic halo of the Milky Way, and the first known substellar subdwarf star. It was discovered from Two Micron All-Sky Survey data, and verified by observations at Palomar Observatory and W. M. Keck Observatory. It has a low metallicity, which indicates it is an old star.

<span class="mw-page-title-main">Planetary-mass object</span> Size-based definition of celestial objects

A planetary-mass object (PMO), planemo, or planetary body is, by geophysical definition of celestial objects, any celestial object massive enough to achieve hydrostatic equilibrium, but not enough to sustain core fusion like a star.

2MASS J21392676+0220226 is a brown dwarf located 34 light-years from Earth in the constellation Aquarius. Its surface is thought to be host to a massive storm, resulting in large variability of its color. It is a member of the Carina-Near moving group. This brown dwarf was discovered in the Two Micron All-Sky Survey (2MASS).

2MASS J03552337+1133437 is a nearby brown dwarf of spectral type L5γ, located in constellation Taurus at approximately 29.8 light-years from Earth.

<span class="mw-page-title-main">Disk Detective</span> NASA-citizen science project

Disk Detective is the first NASA-led and funded-collaboration project with Zooniverse. It is NASA's largest crowdsourcing citizen science project aiming at engaging the general public in search of stars, which are surrounded by dust-rich circumstellar disks, where planets usually dwell and are formed. Initially launched by NASA Citizen Science Officer, Marc Kuchner, the principal investigation of the project was turned over to Steven Silverberg.

<span class="mw-page-title-main">WISE J080822.18-644357.3</span> Red dwarf star in the constellation Carina

WISE J080822.18-644357.3, also called J0808, is a 45+11
−7 Myr old star system in the Carina constellation with a circumstellar debris disk orbiting an M-type red dwarf about 331 lightyears from Earth.

<span class="mw-page-title-main">Backyard Worlds</span> NASA-funded citizen science project

Backyard Worlds: Planet 9 is a NASA-funded citizen science project which is part of the Zooniverse web portal. It aims to discover new brown dwarfs, faint objects that are less massive than stars, some of which might be among the nearest neighbors of the Solar System, and might conceivably detect the hypothesized Planet Nine. The project's principal investigator is Marc Kuchner, an astrophysicist at NASA's Goddard Space Flight Center.

<span class="mw-page-title-main">CI Tauri</span> Star in the constellation Taurus

CI Tauri is a young star, about 2 million years old, located approximately 500 light years away in the constellation Taurus. It is still accreting material from a debris disk at an unsteady pace, possibly modulated by the eccentric orbital motion of the inner planet. The spectral signatures of compounds of sulfur were detected from the disk.

2MASS J11263991−5003550(2MASS J1126−5003) is a brown dwarf about 53 light-years distant from earth. The brown dwarf is notable for an unusual blue near-infrared color. This brown dwarf does not show subdwarf features and the blue color cannot be explained by an unresolved binary. Instead the blue color is explained by patchy clouds. The patchy cloud model allows thick clouds and a cloud coverage of 50% to explain the spectra of 2MASS J1126−5003. Other blue L-dwarfs exist, but are quite rare.

<span class="mw-page-title-main">Tucana-Horologium association</span> Large stellar association

The Tucana-Horologium association (Tuc-Hor), or Tucana Horologium moving group, is a stellar association with an age of 45 ± 4 Myr and it is one of the largest stellar associations within 100 parsecs. The association has a similar size to the Beta Pictoris moving group (BPMG) and contains, like BPMG, more than 12 stars with spectral type B, A and F. The association is named after two southern constellations, the constellation Tucana and the constellation Horologium.

<span class="mw-page-title-main">DL Tauri</span> Protostar system with planetary system in the constellation of Taurus

DL Tauri is a young T Tauri-type pre-main sequence stars in the constellation of Taurus about 522 light years away, belonging to the Taurus Molecular Cloud. It is partially obscured by the foreground gas cloud rich in carbon monoxide, and is still accreting mass, producing 0.14 L☉ due to release of accretion energy. The stellar spectrum shows the lines of ionized oxygen, nitrogen, sulfur and iron.

HD 194012 is a star in the equatorial constellation Delphinus. It has an apparent magnitude of 6.15, making it visible to the naked eye under ideal conditions. The star is relatively close at a distance of only 85 light years but is receding with a heliocentric radial velocity of 4.5 km/s.

<span class="mw-page-title-main">WISEA J120037.79-784508.3</span> Brown dwarf in the constellation Chamaleon


WISEA J120037.79-784508.3, also called W1200-7845 or 2MASS J12003792-7845082, is a brown dwarf with a primordial disk 333.73 ± 3.13 lightyears from Earth in the 3.7+4.6
−1.4 Myr-old ε Chamaeleontis association, currently making it the closest known brown dwarf with an associated circumstellar disk. It was discovered by citizen scientists in 2020 volunteering for the Disk Detective project.

References

  1. 1 2 3 4 5 6 silverbergastro (2020-01-17). "Our New Paper: "Peter Pan Disks"!". Disk Detective. Retrieved 2020-01-22.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 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. 1 2 3 4 5 6 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. 1 2 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. Bibcode:2022ApJ...935..111L. doi: 10.3847/1538-4357/ac8156 . ISSN   0004-637X.
  10. 1 2 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. 1 2 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. 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 . ISSN   0004-6256.
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