Peter Pan disk

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

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] 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] A detailed study of J0446B with JWST MIRI detected 9 hydrocarbons, two nitrogen-bearing species, two isotopes of CO2, molecular hydrogen and two noble gases. Neon and molecular hydrogen strongly supports the idea that this disk is a long-lived primordial disk.[14]

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.[15] 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.[16] 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.[17]

Known Peter Pan disks

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.[18]

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][19] 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.[20]

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.[21] 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.[22] One team also found old accreting stars in the Large Magellanic Cloud in the Tarantula Nebula.[23] This might be explained with a low metallicity in the LMC, which can lead to more massive disks that are less opaque.[15]

List of Peter Pan disk candidates

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][24]
2MASS J02265658-5327032 45±4 Tucana-Horologium association L0δ yes yes [2][24]
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][25]
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][25]
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 [26][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 [25][27][28]

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

There are different models to explain the existence of Peter Pan disks, such as disrupted planetesimals[4] or recent collisions of planetary bodies.[29] 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.[30]

See also

References

  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.
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Maria GorettiDitulis olehFranco BerniniSutradaraGiulio BasePenata musikAndrea MorriconeEnnio MorriconeBahasa asliItaliaProduksiProduserLuca BernabeiSinematografiFabrizio LucciPenyuntingRoberto SicilianoDurasi100 menitRilis asliJaringanRai 1Rilis2003 Maria Goretti adalah sebuah film televisi Italia 2003 yang disutradarai oleh Giulio Base dan dibintangi oleh Martina Pinto dalam peran utama. Film tersebut berdasarkan pada kisah nyata martir-perawan dan Santa Katolik Roma Maria Goretti. ...

Operation Flipper

WW2 British commando raid (Nov 1941), in North Africa Operation Flipper or the 'Rommel Raid'Part of Operation Crusader during the Second World WarGeoffrey Keyes VCDate10–18 November 1941LocationLibya32°55′59″N 21°44′30″E / 32.93306°N 21.74167°E / 32.93306; 21.74167Result Axis victoryBelligerents  United Kingdom  Germany ItalyCommanders and leaders Robert Laycock Geoffrey Keyes † Erwin Rommel Alfredo MercuroCasualties and losses 2...

 

Forever (The Little Dippers song)

1960 single by The Little DippersForeverSingle by The Little DippersB-sideTwo By FourReleasedJanuary 1960RecordedFall 1959GenreEasy listeningLength2:18LabelUniversity RecordsSongwriter(s)Buddy KillenProducer(s)Buddy Killen Forever is a song written by Buddy Killen,[1] which was released by The Little Dippers and Billy Walker in January 1960.[2] Background and chart performance Using the pseudonym The Little Dippers, the Anita Kerr Singers recorded Forever in the fall of 1959.&...

 

عبد الغني السيد

عبد الغني السيد معلومات شخصية تاريخ الميلاد 16 يونيو 1908   تاريخ الوفاة 9 ديسمبر 1962 (54 سنة)   مواطنة مصر  الحياة العملية المهنة مغني،  وممثل  اللغة الأم اللهجة المصرية  اللغات العربية،  واللهجة المصرية  تعديل مصدري - تعديل   عبد الغنى السيد (1908 - 9 ديسمبر 1962)...

Wayward Pines

American mystery science fiction television series For the Blake Crouch novels on which the series is based, see The Wayward Pines Trilogy. Wayward PinesGenre Mystery Science fiction Thriller Horror Based onThe Wayward Pines novelsby Blake CrouchDeveloped byChad HodgeStarring Matt Dillon Carla Gugino Toby Jones Shannyn Sossamon Reed Diamond Tim Griffin Charlie Tahan Juliette Lewis Melissa Leo Terrence Howard Jason Patric Nimrat Kaur Josh Helman Tom Stevens Kacey Rohl Hope Davis Djimon Hounsou...

 

法国世界媒体集团

此條目可参照英語維基百科和法語維基百科相應條目来扩充。 (2024年5月29日)若您熟悉来源语言和主题，请协助参考外语维基百科扩充条目。请勿直接提交机械翻译，也不要翻译不可靠、低品质内容。依版权协议，译文需在编辑摘要注明来源，或于讨论页顶部标记{{Translated page}}标签。 法国世界媒体集团[a]原文名称France Médias Monde公司類型国有企业成立2008年4月4日，Ȁ...

 

CREZL

此条目也许具备关注度，但需要可靠的来源来加以彰显。（2023年8月8日）请协助補充可靠来源以改善这篇条目。 CREZL크레즐组合英文名CREZL国籍 韩国职业歌手、跨界組合语言韓語音乐类型Crossover Music出道日期2024年4月11日，​3個月前​（2024-04-11）出道作品《피안화 (Forbidden Love)》代表作品《피안화 (Forbidden Love)》经纪公司CHXXTA COMPANY（2023年至今）现任成员趙珍虎、�...

Prasterone enanthate

Chemical compound Prasterone enanthateClinical dataTrade namesWith estradiol valerate: Gynodian Depot, othersOther namesDHEA enanthate; Prasterone heptanoate; DHEA heptanoate; DHEA-E; EDHEA; SH-90300-D; SH-70833-D (with EVTooltip estradiol valerate); Androst-5-en-3β-ol-17-one 3β-heptanoateRoutes ofadministrationIntramuscular injectionDrug classAndrogen; Anabolic steroid; Androgen ester; Estrogen; NeurosteroidATC codeG03EA03 (WHO) A14AA07 (WHO)Legal statusLegal status In gener...

 

Lublin

Ne doit pas être confondu avec Dublin. Pour les articles homonymes, voir Lublin (homonymie). Lublin Héraldique Drapeau Lublin Administration Pays Pologne Région Lublin Powiat Ville-powiat Maire Krzysztof Żuk Code postal 20-001 à 20-999[1] Indicatif téléphonique international +(48) Indicatif téléphonique local 81 Immatriculation LU Démographie Population 339 770 hab. (2019) Densité 2 304 hab./km2 Population de l'agglomération 640 000 hab. Géographie ...