Circumplanetary disk

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Circumplanetary disk around exoplanet PDS 70c (point-like source on the right side) PDS 70 closeup - eso2111a.jpg
Circumplanetary disk around exoplanet PDS 70c (point-like source on the right side)

A circumplanetary disk (or circumplanetary disc, short CPD) 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 (or exomoons or subsatellites) may form. [1] Such a disk can manifest itself in various ways.

Contents

In August 2018, astronomers reported the probable detection of a circumplanetary disk around CS Cha B. [2] The authors state that "The CS Cha system is the only system in which a circumplanetary disc is likely present as well as a resolved circumstellar disc." [3] In 2020 though, the parameters of CS Cha B were revised, making it an accreting red dwarf star, and making the disk circumstellar. [4]

Candidates around other exoplanets

Possible circumplanetary disks have also been detected around exoplanets, such as J1407b, [5] HD 100546 b, [6] AS 209 b [7] and HD 169142 b [8] or planetary-mass companions (PMC; 10-20 MJ, separation ≥100 AU), such as GSC 06214-00210 b [9] and DH Tauri b. [10]

A disk was detected in sub-mm with ALMA around SR 12 c, a planetary-mass companion. SR 12 c might not have formed from the circumstellar disk material of the host star SR 12, so it might not be considered a true circumplanetary disk. PMC disks are relative common around young objects and are easier to study when compared to circumplanetary disks. [11]

Several disks were detected around nearby isolated planetary-mass objects. Disks around such objects within 300 parsecs were found in Rho Ophiuchi Complex, [12] Taurus Complex (e.g. KPNO-Tau 12), [12] [13] Lupus I Cloud [14] and the Chamaeleon Complex (e.g. the well studied OTS 44 and Cha 110913−773444 [15] ). These objects with disks are free-floating and are most of the time called circumstellar disks, despite likely being similar to circumplanetary disks.

2M1207b was suspected to have a circumplanetary disk in the past. [16] New observations from JWST/NIRSpec were able to confirm accretion from an unseen disk by detecting emission from hydrogen and helium. The classification of a circumplanetary disk is however being disputed because 2M1207b (or 2M1207B) might be classified as a binary together with 2M1207A and not an exoplanet. This would make the disk around 2M1207b a circumstellar disk, despite not being around a star, but around a 5-6 MJup planetary-mass object. [17]

PDS 70

The disk around the planet c of the PDS 70 system is the best evidence for a circumplanetary disk at the time of its discovery. The exoplanet is part of the multiplanetary PDS 70 star system, about 370 light-years (110 parsecs) from Earth. [18]

PDS 70b

In June 2019 astronomers reported the detection of evidence of a circumplanetary disk around PDS 70b [19] using spectroscopy and accretion signatures. Both types of these signatures had previously been detected for other planetary candidates. A later infrared characterization could not confirm the spectroscopic evidence for the disk around PDS 70b and reports weak evidence that the current data favors a model with a single blackbody component. [20]

PDS 70c

In July 2019 astronomers reported the first-ever detection using the Atacama Large Millimeter/submillimeter Array (ALMA) [21] [22] [23] of a circumplanetary disk. [21] [22] [24] ALMA studies, using millimetre and submillimetre wavelengths, are better at observing dust concentrated in interplanetary regions, since stars emit comparatively little light at these wavelengths, and since optical observations are often obscured by overwhelming glare from the bright host star. The circumplanetary disk was detected around a young massive, Jupiter-like exoplanet, PDS 70c. [21] [22] [24]

According to Andrea Isella, lead researcher from the Rice University in Houston, Texas, "For the first time, we can conclusively see the tell-tale signs of a circumplanetary disk, which helps to support many of the current theories of planet formation ... By comparing our observations to the high-resolution infrared and optical images, we can clearly see that an otherwise enigmatic concentration of tiny dust particles is actually a planet-girding disk of dust, the first such feature ever conclusively observed." [23] Jason Wang from Caltech, lead researcher of another publication, describes, "if a planet appears to sit on top of the disk, which is the case with PDS 70c" [25] then the signal around PDS 70c needs to be spatially separated from the outer ring, not the case in 2019. However, in July 2021 higher resolution, conclusively resolved data were presented. [26]

The planet PDS 70c is detected in H-alpha, which is seen as evidence that it accretes material from the circumplanetary disk at a rate of 10−8±0.4 MJ per year. [27] From ALMA observations it was shown that this disk has a radius smaller than 1.2 astronomical units (AU) or a third of the Hill radius. The dust mass was estimated around 0.007 or 0.031 ME (0.57 to 2.5 Moon masses), depending on the grain size used for the modelling. [26] Later modelling showed that the disk around PDS 70c is optically thick and has an estimated dust mass of 0.07 to 0.7 ME (5.7 to 57 Moon masses). The total (dust+gas) mass of the disk should be higher. The planet's luminosity is the dominant heating mechanism within 0.6 AU of the CPD. Beyond that the photons from the star heat the disk. [28]

See also

Related Research Articles

<span class="mw-page-title-main">Protoplanetary disk</span> Gas and dust surrounding a newly formed star

A protoplanetary disk is a rotating circumstellar disc of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig Ae/Be star. The protoplanetary disk may also be considered an accretion disk for the star itself, because gases or other material may be falling from the inner edge of the disk onto the surface of the star. This process should not be confused with the accretion process thought to build up the planets themselves. Externally illuminated photo-evaporating protoplanetary disks are called proplyds.

<span class="mw-page-title-main">Protoplanet</span> Large planetary embryo

A protoplanet is a large planetary embryo that originated within a protoplanetary disk and has undergone internal melting to produce a differentiated interior. Protoplanets are thought to form out of kilometer-sized planetesimals that gravitationally perturb each other's orbits and collide, gradually coalescing into the dominant planets.

<span class="mw-page-title-main">Rogue planet</span> Planetary object 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">2M1207</span> Brown dwarf in the constellation Centaurus

2M1207, 2M1207A or 2MASS J12073346–3932539 is a brown dwarf located in the constellation Centaurus; a companion object, 2M1207b, may be the first extrasolar planetary-mass companion to be directly imaged, and is the first discovered orbiting a brown dwarf.

<span class="mw-page-title-main">2M1207b</span> Planetary-mass object orbiting the brown dwarf 2M1207

2M1207b is a planetary-mass object orbiting the brown dwarf 2M1207, in the constellation Centaurus, approximately 170 light-years from Earth. It is one of the first candidate exoplanets to be directly observed. It was discovered in April 2004 by the Very Large Telescope (VLT) at the Paranal Observatory in Chile by a team from the European Southern Observatory led by Gaël Chauvin. It is believed to be from 5 to 6 times the mass of Jupiter and may orbit 2M1207 at a distance roughly as far from the brown dwarf as Pluto is from the Sun.

<span class="mw-page-title-main">Exomoon</span> Moon beyond the Solar System

An exomoon or extrasolar moon is a natural satellite that orbits an exoplanet or other non-stellar extrasolar body.

<span class="mw-page-title-main">OTS 44</span> Celestial object in the constellation Chamaeleon

OTS 44 is a free-floating planetary-mass object or brown dwarf located at 550 light-years (170 pc) in the constellation Chamaeleon near the reflection nebula IC 2631. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of Jupiter, or approximately 1.1% that of the Sun. Its radius is not very well known and is estimated to be 23–57% that of the Sun.

<span class="mw-page-title-main">Sub-brown dwarf</span> Astronomical objects of planetary size that did not form in orbit around a star

A sub-brown dwarf or planetary-mass brown dwarf is an astronomical object that formed in the same manner as stars and brown dwarfs but that has a planetary mass, therefore by definition below the limiting mass for thermonuclear fusion of deuterium . Some researchers call them rogue planets whereas others call them planetary-mass brown dwarfs. They are sometimes categorized as Y spectral class brown dwarfs.

<span class="mw-page-title-main">HD 100546</span> Star in the constellation Musca

HD 100546, also known as KR Muscae, is a pre-main sequence star of spectral type B8 to A0 located 353 light-years from Earth in the southern constellation of Musca. The star is surrounded by a circumstellar disk from a distance of 0.2 to 4 AU, and again from 13 AU out to a few hundred AU, with evidence for a protoplanet forming at a distance of around 47 AU.

<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">AB Aurigae</span> Star in the constellation Auriga

AB Aurigae is a young Herbig Ae star in the Auriga constellation. It is located at a distance of approximately 531 light years from the Sun based on stellar parallax. This pre-main-sequence star has a stellar classification of A0Ve, matching an A-type main-sequence star with emission lines in the spectrum. It has 2.4 times the mass of the Sun and is radiating 38 times the Sun's luminosity from its photosphere at an effective temperature of 9,772 K. The radio emission from the system suggests the presence of a thermal jet originating from the star with a velocity of 300 km s−1. This is causing an estimated mass loss of 1.7×10−8 M☉ yr−1.

<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">HD 169142</span> Pre-main-sequence star in the constellation Sagittarius

HD 169142 is a single Herbig Ae/Be star. Its surface temperature is 7650±150 K. HD 169142 is depleted of heavy elements compared to the Sun, with a metallicity Fe/H index of −0.375±0.125, but is much younger at an age of 7.5±4.5 million years. The star is rotating slowly and has relatively low stellar activity for a Herbig Ae/Be star.

<span class="mw-page-title-main">LkCa 15</span> Star system in the constellation Taurus

LkCa 15 is a T Tauri star in the Taurus Molecular Cloud. These types of stars are relatively young pre-main-sequence stars that show irregular variations in brightness. It has a mass that is about 97% of the Sun, an effective temperature of 4370 K, and is slightly cooler than the Sun. Its apparent magnitude is 11.91, meaning it is not visible to the naked eye.

<span class="mw-page-title-main">PDS 70</span> T Tauri-type star in the constellation Centaurus

PDS 70 is a very young T Tauri star in the constellation Centaurus. Located 370 light-years from Earth, it has a mass of 0.76 M☉ and is approximately 5.4 million years old. The star has a protoplanetary disk containing two nascent exoplanets, named PDS 70b and PDS 70c, which have been directly imaged by the European Southern Observatory's Very Large Telescope. PDS 70b was the first confirmed protoplanet to be directly imaged.

<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 523 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 an inner planet. The spectral signatures of compounds of sulfur were detected from the disk.

<span class="mw-page-title-main">LSPM J0207+3331</span> Star in the constellation Taurus

LSPM J0207+3331 is, as of 2023, the oldest and coldest known white dwarf star to host a circumstellar disk, located 145 light-years from Earth. It was discovered in October 2018 by a volunteer participating in the Backyard Worlds citizen science project.

References

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  2. ↑ Ginski, Christian (August 2018). "First direct detection of a polarized companion outside a resolved circumbinary disk around CS Chamaeleonis". Astronomy & Astrophysics . 616 (79): 18. arXiv: 1805.02261 . Bibcode:2018A&A...616A..79G. doi: 10.1051/0004-6361/201732417 .
  3. ↑ Starr, Michelle. "Astronomers Have Accidentally Taken a Direct Photo of a Possible Baby Exoplanet" . Retrieved 10 October 2019.
  4. ↑ Haffert, S. Y.; Van Holstein, R. G.; Ginski, C.; Brinchmann, J.; Snellen, I. A. G.; Milli, J.; Stolker, T.; Keller, C. U.; Girard, J. (2020), "CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion", Astronomy & Astrophysics, 640: L12, arXiv: 2007.07831 , Bibcode:2020A&A...640L..12H, doi:10.1051/0004-6361/202038706, S2CID   220525346
  5. ↑ Mamajek, Eric E.; et al. (March 2012). "Planetary Construction Zones in Occultation: Discovery of an Extrasolar Ring System Transiting a Young Sun-like Star and Future Prospects for Detecting Eclipses by Circumsecondary and Circumplanetary Disks". The Astronomical Journal . 143 (3): 72. arXiv: 1108.4070 . Bibcode:2012AJ....143...72M. doi:10.1088/0004-6256/143/3/72. S2CID   55818711.
  6. ↑ Quanz, Sascha P.; et al. (July 2015). "Confirmation and Characterization of the Protoplanet HD 100546 b—Direct Evidence for Gas Giant Planet Formation at 50 AU". The Astrophysical Journal . 807 (1): 64. arXiv: 1412.5173 . Bibcode:2015ApJ...807...64Q. doi:10.1088/0004-637X/807/1/64. S2CID   119119314.
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  16. ↑ Mohanty, Subhanjoy; et al. (March 2007). "The Planetary Mass Companion 2MASS 1207-3932B: Temperature, Mass, and Evidence for an Edge-on Disk". The Astrophysical Journal . 657 (2): 1064–1091. arXiv: astro-ph/0610550 . Bibcode:2007ApJ...657.1064M. doi:10.1086/510877. S2CID   17326111.
  17. ↑ Luhman, K. L.; Tremblin, P.; Birkmann, S. M.; Manjavacas, E.; Valenti, J.; Alves de Oliveira, C.; Beck, T. L.; Giardino, G.; Lützgendorf, N.; Rauscher, B. J.; Sirianni, M. (1 June 2023). "JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B". The Astrophysical Journal. 949 (2): L36. arXiv: 2305.18603 . Bibcode:2023ApJ...949L..36L. doi: 10.3847/2041-8213/acd635 . ISSN   0004-637X.
  18. ↑ Mandelbaum, Ryan F. (12 July 2019). "Astronomers Think They've Spotted a Moon Forming Around an Exoplanet". Gizmodo . Retrieved 12 July 2019.
  19. ↑ Christiaens, Valentin (June 2019). "Evidence for a circumplanetary disk around protoplanet PDS 70 b". The Astrophysical Journal Letters . 877 (2): L33. arXiv: 1905.06370 . Bibcode:2019ApJ...877L..33C. doi: 10.3847/2041-8213/ab212b . S2CID   155100321.
  20. ↑ Stolker, T.; Marleau, G.-D.; Cugno, G.; Mollière, P.; Quanz, S. P.; Todorov, K. O.; Kühn, J. (December 2020). "MIRACLES: atmospheric characterization of directly imaged planets and substellar companions at 4–5 μ m: II. Constraints on the mass and radius of the enshrouded planet PDS 70 b". Astronomy & Astrophysics. 644: A13. arXiv: 2009.04483 . Bibcode:2020A&A...644A..13S. doi: 10.1051/0004-6361/202038878 . ISSN   0004-6361.
  21. 1 2 3 Isella, Andrea; et al. (11 July 2019). "Detection of Continuum Submillimeter Emission Associated with Candidate Protoplanets". The Astrophysical Journal Letters . 879 (2): L25. arXiv: 1906.06308 . Bibcode:2019ApJ...879L..25I. doi: 10.3847/2041-8213/ab2a12 . S2CID   189897829.
  22. 1 2 3 Blue, Charles E. (11 July 2019). "'Moon-forming' Circumplanetary Disk Discovered in Distant Star System". National Radio Astronomy Observatory . Retrieved 11 July 2019.
  23. 1 2 Carne, Nick (13 July 2019). "'Moon-forming' disk found in distant star system - Discovery helps confirm theories of planet formation, astronomers say". Cosmos . Archived from the original on 12 July 2019. Retrieved 12 July 2019.
  24. 1 2 Boyd, Jade (11 July 2019). "Moon-forming disk discovered around distant planet". Phys.org . Retrieved 11 July 2019.
  25. ↑ Observatory, W. M. Keck. "Astronomers confirm existence of two giant newborn planets in PDS 70 system". phys.org. Retrieved 27 July 2022.
  26. 1 2 Benisty, Myriam; Bae, Jaehan; Facchini, Stefano; Keppler, Miriam; Teague, Richard; Isella, Andrea; Kurtovic, Nicolas T.; Pérez, Laura M.; Sierra, Anibal; Andrews, Sean M.; Carpenter, John (1 July 2021). "A Circumplanetary Disk around PDS70c". The Astrophysical Journal Letters. 916 (1): L2. arXiv: 2108.07123 . Bibcode:2021ApJ...916L...2B. doi: 10.3847/2041-8213/ac0f83 . ISSN   2041-8205. S2CID   236186222.
  27. ↑ Haffert, S. Y.; Bohn, A. J.; de Boer, J.; Snellen, I. A. G.; Brinchmann, J.; Girard, J. H.; Keller, C. U.; Bacon, R. (1 June 2019). "Two accreting protoplanets around the young star PDS 70". Nature Astronomy. 3: 749–754. arXiv: 1906.01486 . doi:10.1038/s41550-019-0780-5. ISSN   2397-3366.
  28. ↑ Portilla-Revelo, B.; Kamp, I.; Rab, Ch.; van Dishoeck, E. F.; Keppler, M.; Min, M.; Muro-Arena, G. A. (1 February 2022). "Self-consistent modelling of the dust component in protoplanetary and circumplanetary disks: the case of PDS 70". Astronomy and Astrophysics. 658: A89. arXiv: 2111.08648 . doi:10.1051/0004-6361/202141764. ISSN   0004-6361.
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