Debris disk

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Hubble Space Telescope observation of the debris ring around Fomalhaut. The inner edge of the disk may have been shaped by the orbit of Fomalhaut b, at lower right. Fomalhaut with Disk Ring and extrasolar planet b.jpg
Hubble Space Telescope observation of the debris ring around Fomalhaut. The inner edge of the disk may have been shaped by the orbit of Fomalhaut b, at lower right.

A debris disk (American English), or debris disc (Commonwealth English), is a circumstellar disk of dust and debris in orbit around a star. Sometimes these disks contain prominent rings, as seen in the image of Fomalhaut on the right. Debris disks are found around stars with mature planetary systems, including at least one debris disk in orbit around an evolved neutron star. [1] Debris disks can also be produced and maintained as the remnants of collisions between planetesimals, otherwise known as asteroids and comets. [2]

Contents

As of 2001, more than 900 candidate stars had been found to possess a debris disk. They are usually discovered by examining the star system in infrared light and looking for an excess of radiation beyond that emitted by the star. This excess is inferred to be radiation from the star that has been absorbed by the dust in the disk, then re-radiated away as infrared energy. [3]

Debris disks are often described as massive analogs to the debris in the Solar System. Most known debris disks have radii of 10–100 astronomical units (AU); they resemble the Kuiper belt in the Solar System, although the Kuiper belt does not have a high enough dust mass to be detected around even the nearest stars. Some debris disks contain a component of warmer dust located within 10 AU from the central star. This dust is sometimes called exozodiacal dust by analogy to zodiacal dust in the Solar System.

Observation history

VLT and Hubble images of the disc around AU Microscopii. VLT and Hubble images of the disc around AU Microscopii.jpg
VLT and Hubble images of the disc around AU Microscopii.

In 1984 a debris disk was detected around the star Vega using the IRAS satellite. Initially this was believed to be a protoplanetary disk, but it is now known to be a debris disk due to the lack of gas in the disk and the age of the star. The first four debris disks discovered with IRAS are known as the "fabulous four": Vega, Beta Pictoris, Fomalhaut, and Epsilon Eridani. Subsequently, direct images of the Beta Pictoris disk showed irregularities in the dust, which were attributed to gravitational perturbations by an unseen exoplanet. [5] That explanation was confirmed with the 2008 discovery of the exoplanet Beta Pictoris b. [6]

Other exoplanet-hosting stars, including the first discovered by direct imaging (HR 8799), are known to also host debris disks. The nearby star 55 Cancri, a system that is also known to contain five planets, also was reported to have a debris disk, [7] but that detection could not be confirmed. [8] Structures in the debris disk around Epsilon Eridani suggest perturbations by a planetary body in orbit around that star, which may be used to constrain the mass and orbit of the planet. [9]

On 24 April 2014, NASA reported detecting debris disks in archival images of several young stars, HD 141943 and HD 191089, first viewed between 1999 and 2006 with the Hubble Space Telescope, by using newly improved imaging processes. [10]

In 2021, observations of a star, VVV-WIT-08, that became obscured for a period of 200 days may have been the result of a debris disk passing between the star and observers on Earth. [11] Two other stars, Epsilon Aurigae and TYC 2505-672-1, are reported to be eclipsed regularly and it has been determined that the phenomenon is the result of disks orbiting them in varied periods, suggesting that VVV-WIT-08 may be similar and have a much longer orbital period that just has been experienced by observers on Earth. VVV-WIT-08 is ten times the size of the Sun in the constellation of Sagittarius.

Origin

Debris disks detected in HST archival images of young stars, HD 141943 and HD 191089, using improved imaging processes (24 April 2014). NASA-14114-HubbleSpaceTelescope-DebrisDisks-20140424.jpg
Debris disks detected in HST archival images of young stars, HD 141943 and HD 191089, using improved imaging processes (24 April 2014).

During the formation of a Sun-like star, the object passes through the T-Tauri phase during which it is surrounded by a gas-rich, disk-shaped nebula. Out of this material are formed planetesimals, which can continue accreting other planetesimals and disk material to form planets. The nebula continues to orbit the pre-main-sequence star for a period of 1–20 million years until it is cleared out by radiation pressure and other processes. Second generation dust may then be generated about the star by collisions between the planetesimals, which forms a disk out of the resulting debris. At some point during their lifetime, at least 45% of these stars are surrounded by a debris disk, which then can be detected by the thermal emission of the dust using an infrared telescope. Repeated collisions may cause a disk to persist for much of the lifetime of a star. [12]

Typical debris disks contain small grains 1–100  μm in size. Collisions will grind down these grains to sub-micrometre sizes, which will be removed from the system by radiation pressure from the host star. In very tenuous disks such as the ones in the Solar System, the Poynting–Robertson effect can cause particles to spiral inward instead. Both processes limit the lifetime of the disk to 10  Myr or less. Thus, for a disk to remain intact, a process is needed to continually replenish the disk. This can occur, for example, by means of collisions between larger bodies, followed by a cascade that grinds down the objects to the observed small grains. [13]

For collisions to occur in a debris disk, the bodies must be gravitationally perturbed sufficiently to create relatively large collisional velocities. A planetary system around the star can cause such perturbations, as can a binary star companion or the close approach of another star. [13] The presence of a debris disk may indicate a high likelihood of exoplanets orbiting the star. [14] Furthermore, many debris disks also show structures within the dust (for example, clumps and warps or asymmetries) that point to the presence of one or more exoplanets within the disk. [6] The presence or absence of asymmetries in our own trans-Neptunian belt remains controversial although they might exist. [15]

Extreme Debris disks

A sub-type of debris disk is the so-called "extreme debris disk" (EDD). This type is defined as exceeding 1% of the luminosity of the star in the infrared. An EDD is surrounded by warm dust (200-600 Kelvin), that orbits the star within a few astronomical units. In other words the dust is present in a region where terrestrial planets form. EDDs are rare and around 24 are known as of 2024. Infrared spectra with Spitzer have shown that the dust is dominated by small particles made up of silicates that have a size between sub-μm and a few μm. EDDs are interpreted to have formed from one or more giant collisions between large planetesimals or planetary bodies. This is different to most debris disks, which are sustained by smaller collisions. [16] EDDs are often transient events, with the dust produced in the event lasting years around the star before radiation pressure blows the small particles away. 2MASS J08090250-4858172 was one of the first such systems with observed infrared variability, showing two giant impact events in 2012 and 2014. [17] In rare cases the dust cloud can orbit in front of the star, causing dips of brightness in the optical. One such system is HD 166191, which shows a star-sized dust cloud transiting in front of the star. [18] Giant impacts are more common in young systems and after around 300 Myrs giant impacts become less common. A few relative old EDDs are also known, reaching up to 5.5 Gyrs. These old EDDs often have a wide, eccentric companion, which might help trigger such giant impact events. [16] Giant impacts might not always be detectable as EDDs. Such disks are made up of two types of dust. The first type is vapor condensates that is produced immediately in the event. The second type is dust created by the grinding down of boulders produced in the event. Simulations have shown that boulders are more important to classify disks as extreme. [19]

Known belts

Belts of dust or debris have been detected around many stars, including the Sun, including the following:

Star Spectral
class [20] 		Distance
(ly)		Orbit
(AU)		Notes
Epsilon Eridani K2V10.535–75 [9]
Tau Ceti G8V11.935–50 [21]
Vega A0V2586–200 [22] [23]
Fomalhaut A3V25133–158 [22]
AU Microscopii M1Ve3350–150 [24]
HD 181327 F5.5V51.889-110 [25]
HD 69830 K0V41<1 [26]
HD 207129 G0V52148–178 [27]
HD 139664 F5IV–V5760–109 [28]
Eta Corvi F2V59100–150 [29]
HD 53143 K1V60 ? [28]
Beta Pictoris A6V6325–550 [23]
Zeta Leporis A2Vann702–8 [30]
HD 92945 K1V7245–175 [31]
HD 107146 G2V88130 [32]
Gamma Ophiuchi A0V95520 [33]
HR 8799 A5V12975 [34]
51 Ophiuchi B91310.5–1200 [35]
HD 12039 G3–5V1375 [36]
HD 98800 K5e (?)1501 [37]
HD 15115 F2V150315–550 [38]
HR 4796  AA0V220200 [39] [40]
HD 141569 B9.5e320400 [40]
HD 113766 AF4V4300.35–5.8 [41]
HD 141943 [10]
HD 191089 [10]

The orbital distance of the belt is an estimated mean distance or range, based either on direct measurement from imaging or derived from the temperature of the belt. The Earth has an average distance from the Sun of 1 AU.

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 not be considered an accretion disk; while the two are similar, an accretion disk is hotter and spins much faster. It is also found on black holes, not stars. 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">Beta Pictoris</span> Second brightest star in the southern constellation of Pictor

Beta Pictoris is the second brightest star in the constellation Pictor. It is located 63.4 light-years (19.4 pc) from the Solar System, and is 1.75 times as massive and 8.7 times as luminous as the Sun. The Beta Pictoris system is very young, only 20 to 26 million years old, although it is already in the main sequence stage of its evolution. Beta Pictoris is the title member of the Beta Pictoris moving group, an association of young stars which share the same motion through space and have the same age.

<span class="mw-page-title-main">AU Microscopii</span> Star in the constellation Microscopium

AU Microscopii is a young red dwarf star located 31.7 light-years away – about 8 times as far as the closest star after the Sun. The apparent visual magnitude of AU Microscopii is 8.73, which is too dim to be seen with the naked eye. It was given this designation because it is in the southern constellation Microscopium and is a variable star. Like β Pictoris, AU Microscopii has a circumstellar disk of dust known as a debris disk and at least two exoplanets, with the presence of an additional two planets being likely.

<span class="mw-page-title-main">HD 107146</span> Star in the constellation Coma Berenices

HD 107146 is a star in the constellation Coma Berenices that is located about 90 light-years (28 pc) from Earth. The apparent magnitude of 7.028 makes this star too faint to be seen with the unaided eye.

<span class="mw-page-title-main">HD 10647</span> Star in the constellation Eridanus

HD 10647 is a 6th-magnitude yellow-white dwarf star, 57 light-years away in the constellation of Eridanus. The star is visible to the unaided eye under very dark skies. It is slightly hotter and more luminous than the Sun, and at 1.75 billion years old, it is also younger. An extrasolar planet was discovered orbiting this star in 2003.

HD 210277 is a single star in the equatorial constellation of Aquarius. It has an apparent visual magnitude of 6.54, which makes it a challenge to view with the naked eye, but it is easily visible in binoculars. The star is located at a distance of 69.6 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −20.9 km/s.

HD 69830 is a yellow dwarf star located 41.0 light-years away in the constellation of Puppis. In 2005, the Spitzer Space Telescope discovered a narrow ring of warm debris orbiting the star. The debris ring contains substantially more dust than the Solar System's asteroid belt. In 2006, three extrasolar planets with minimum masses comparable to Neptune were confirmed in orbit around the star, located interior to the debris ring.

Eta Telescopii is a white-hued star in the southern constellation of Telescopium. This is an A-type main sequence star with an apparent visual magnitude of +5.03. It is approximately 158 light years from Earth and is a member of the Beta Pictoris Moving Group of stars that share a common motion through space. It forms a wide binary system with the star HD 181327 and has a substellar companion orbiting around it, named Eta Telescopii B.

<span class="mw-page-title-main">HD 12039</span> Star in the constellation Cetus

HD 12039, also known as DK Ceti, is a variable star in the constellation of Cetus at a distance of 135 ly (41 pc). It is categorized as a BY Draconis variable because of luminosity changes caused by surface magnetic activity coupled with rotation of the star. The stellar classification G4V is similar to the Sun, indicating this is a main sequence star that is generating energy at its core through the thermonuclear fusion of hydrogen. The effective temperature of 5,585 K gives the star a yellow hue. It has about the same mass as the Sun, but only emits 89% of the Sun's luminosity. This is a young star with age estimates ranging from 7.5−8 million years to 30 million years.

<span class="mw-page-title-main">Methods of detecting exoplanets</span>

Any planet is an extremely faint light source compared to its parent star. For example, a star like the Sun is about a billion times as bright as the reflected light from any of the planets orbiting it. In addition to the intrinsic difficulty of detecting such a faint light source, the light from the parent star causes a glare that washes it out. For those reasons, very few of the exoplanets reported as of January 2024 have been observed directly, with even fewer being resolved from their host star.

<span class="mw-page-title-main">Eta Corvi</span> Star in the constellation of Corvus

Eta Corvi is an F-type main-sequence star, the sixth-brightest star in the constellation of Corvus. Two debris disks have been detected orbiting this star, one at ~150 AU, and a warmer one within a few astronomical units (AU).

<span class="mw-page-title-main">HD 53143</span> Star in the constellation Carina

HD 53143 is a star in the Carina constellation, located about 59.8 light-years from the Earth. With an apparent visual magnitude of 6.80, this star is a challenge to view with the naked eye even under ideal viewing conditions.

HD 98800, also catalogued as TV Crateris, is a quadruple star system in the constellation of Crater. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 150 light-years away. The system is located within the TW Hydrae association (TWA), and has received the designation TWA 4.

<span class="mw-page-title-main">HD 113766</span> Binary star in the constellation Centaurus

HD 113766 is a binary star system located 424 light years from Earth in the direction of the constellation Centaurus. The star system is approximately 10 million years old and both stars are slightly more massive than the Sun. The two are separated by an angle of 1.3 arcseconds, which, at the distance of this system, corresponds to a projected separation of at least 170 AU.

<span class="mw-page-title-main">HD 141569</span> Star in the constellation Libra

HD 141569 is an isolated Herbig Ae/Be star of spectral class A2Ve approximately 364 light-years away in the constellation of Libra. The primary star has two red dwarf companions at about nine arcseconds. In 1999, a protoplanetary disk was discovered around the star. A gap in the disk led to speculation about a possible extrasolar planet forming in the disk.

<span class="mw-page-title-main">HD 172555</span> Star in the constellation Pavo

HD 172555 is a white-hot Type A7V star located relatively close by, 95 light years from Earth in the direction of the constellation Pavo. Spectrographic evidence indicates a relatively recent collision between two planet-sized bodies that destroyed the smaller of the two, which had been at least the size of the Moon, and severely damaged the larger one, which was at least the size of Mercury. Evidence of the collision was detected by NASA's Spitzer Space Telescope.

<span class="mw-page-title-main">Paul Kalas</span> Greek American astronomer (born 1967)

Paul Kalas is a Greek American astronomer known for his discoveries of debris disks around stars. Kalas led a team of scientists to obtain the first visible-light images of an extrasolar planet with orbital motion around the star Fomalhaut, at a distance of 25 light years from Earth. The planet is referred to as Fomalhaut b.

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

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<span class="mw-page-title-main">Circumstellar disc</span> Accumulation of matter around a star

A circumstellar disc is a torus, pancake or ring-shaped accretion disk of matter composed of gas, dust, planetesimals, asteroids, or collision fragments in orbit around a star. Around the youngest stars, they are the reservoirs of material out of which planets may form. Around mature stars, they indicate that planetesimal formation has taken place, and around white dwarfs, they indicate that planetary material survived the whole of stellar evolution. Such a disc can manifest itself in various ways.

References

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  39. ↑ Koerner, D. W.; Ressler, M. E.; Werner, M. W.; Backman, D. E. (1998). "Mid-Infrared Imaging of a Circumstellar Disk around HR 4796: Mapping the Debris of Planetary Formation". Astrophysical Journal Letters. 503 (1): L83. arXiv: astro-ph/9806268 . Bibcode:1998ApJ...503L..83K. doi:10.1086/311525. S2CID   12715138.
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  41. ↑ Meyer, M. R.; Backman, D. (2002-01-08). "Belt of Material Around Star May Be First Step in Terrestrial Planet Formation". University of Arizona, NASA. Archived from the original on 2011-06-07. Retrieved 2007-07-17.
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