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] 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

Peter Pan disk.png
Artist's Impression of a Peter Pan disk
PDS 111 SPHERE A&A, 688, A149 (2024).png
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

NameAge (Myrs)Associationspectral typeinfrared excessaccretionReference
WISE J080822.18-644357.3 45+11
−7		Carina associationM5yesyes [3] [4]
2MASS J05010082-4337102 42+6
−4		 Columba association M4.5yesyes [2] [23]
2MASS J02265658-5327032 45±4 Tucana-Horologium association L0δyesyes [2] [23]
WISEA J044634.16-262756.1 42+6
−4		Columba association (but might be χ1 Fornacis member, which is 34 Myr old)M6+M6yeslikely [2] [24]
WISEA J094900.65-713803.1 45+11
−7		Carina associationM4+M5yesyes both [2]
2MASS J15460752-6258042 ~55 Argus association (but might be Beta Pictoris member)M5yesyes [10] [24]
2MASS J05082729−2101444 30-44Columba association (but could be Beta Pictoris member)M5yesyes [10]
LDS 5606 30-44Columba association (but could be Beta Pictoris member)M5+M5yesyes [25] [10]
Delorme 1 (AB)b30-45Tucana-Horologium associationL0 (very low gravity)noyes [7] [12] [13]
2MASS J06320799-6810419 ~45Carina associationM4.5yesyes [9]
2MASS J19150079-2847587 24±3 Beta Pictoris moving group M4.8 (binary candidate)yesyes [11]
StHα34 24.7+0.9
−0.6		Beta Pictoris moving groupM3+M3yesyes [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

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

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 fuse lithium (7Li).

<span class="mw-page-title-main">Proplyd</span> Dust ring surrounding large stars thousands of solar radii wide

A proplyd, short for ionized protoplanetary disk, is an externally illuminated photoevaporating protoplanetary disk around a young star. Nearly 180 proplyds have been discovered in the Orion Nebula. Images of proplyds in other star-forming regions are rare, while Orion is the only region with a large known sample due to its relative proximity to Earth.

<span class="mw-page-title-main">Rogue planet</span> Planets not gravitationally bound to a star

A rogue planet, 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.

<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.

<span class="mw-page-title-main">Exocomet</span> Comet outside the Solar System

An exocomet, or extrasolar comet, is a comet outside the Solar System, which includes rogue comets and comets that orbit stars other than the Sun. The first exocomets were detected in 1987 around Beta Pictoris, a very young A-type main-sequence star. There are now a total of 27 stars around which exocomets have been observed or suspected.

<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">Circumplanetary disk</span> Accumulation of matter around a planet

A circumplanetary disk is a torus, pancake or ring-shaped accumulation of matter composed of gas, dust, planetesimals, asteroids or collision fragments in orbit around a planet. They are reservoirs of material out of which moons may form. Such a disk can manifest itself in various ways.

<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.

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">Delorme 1</span> Binary star system in the Phoenix constellation

Delorme 1 is a binary star with a planetary-mass companion (PMC) or protoplanet in a circumbinary orbit. The PMC is notable for showing signs of accretion, despite being 30-45 Myr old, making it similar to Peter Pan disks. These disks show characteristics of a gas-rich disk at unexpected high ages.

References

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  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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