1. Observational evidence for accretion discs in the Universe - davidar/scholarpedia GitHub Wiki
== Accretion discs in young stellar objects (YSOs) ==
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During star formation, the central part of a dense molecular cloud collapses
to a proto-star with a gaseous envelope that finally settles to a rotating
proto-planetary accretion disc. Sedimentation and self-gravity in such discs
trigger the formation of planets and planetary systems.
Proto-stars are heavily embedded in surrounding gas and dust and for this reason
visible only in the infrared, millimetre or sub-millimetre wavelength bands.
Most of the material that goes into forming a star is accreted through a circumstellar
disc and in this process the proto-stellar system drives an energetic bipolar jet
and outflow into its surroundings. The least evolved proto-stars are surrounded by
remnant proto-planetary accretion discs.
Based on the spectral energy distribution in the infrared and visible light, YSOs are divided into five classes (0-IV), associated with their evolutionary stages. Class 0 refers to collapsing molecular clouds, proto-planetary discs exist in classes I-III, and class IV contains the zero-age main-sequence star. *[http://www.circumstellardisks.org/ '''Catalog of Resolved Circumstellar Disks''' maintained by Caer McCabe & Carlotta Pham] *[http://cfa-www.harvard.edu/rg/star_and_planet_formation/young_stellar_objects.html Harvard University Research Group (Young Stellar Objects)] *[http://arxiv.org/abs/astro-ph/0607387 Roy van Boekel et al., 2006, ''Disks around young stars with VLTI-MIDI''] *[http://arxiv.org/abs/astro-ph/0409190 R.D. Blum et al., 2004, ''Accretion Signatures from Massive Young Stellar Objects''] A related issue: the extrasolar planets *[http://exoplanet.eu/ ''The Extrasolar Planets Encyclopaedia'', maintained by Jean Schneider CNRS/LUTH - Paris Observatory ] |
Accretion disc and jet in a proto-star
HH30 observed by the Hubble Space Telescope:
the jet (in red) is perpendicular to the accretion disc, seen edge-on (a dark region between two bright lobes),
© Burrows, STSci/ESA, WFPC2, NASA)
|frame|283px|A proto-star star in NGC 1333. Reconstruction of
a possible look of a proto-planetery disk based on a Spitzer Space Telescope image. An evidence
was found for water vapor in the surrounding area, which appears to be
one of the key moments in the development of a planetary system around such a star: icy material
is falling from the envelope that birthed the star onto a dense, surrounding disc.
Credit: NASA/JPL-Caltech/R. Gutermuth (Harvard-Smithsonian Center for Astrophysics)]]== Accretion discs in cataclysmic variables (CVs) ==
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[[Image:Ugem-model.gif|frame|480px|left|U Gem system, as it would be seen from the Earth. In reality, the image of the system is unresolved, and only the total flux from the secondary (red) and accretion disc (blue) is observed. The primary white dwarf is located at the centre of the accretion disc (too small to be seen). The secondary and the accretion disc periodically eclipse each other, which results in periodic variations in the observed flux (photometry) and spectral features (spectroscopy). From these variations [http://adsabs.harvard.edu/abs/1971AcA....21...15S Smak (1971)] reconstructed size and shape of the accretion disc.]] |
CVs are binary star systems consisting of a white dwarf ("primary") and a normal star ("secondary", or "companion"). Typically, the CVs have sizes comparable to the Earth-Moon system, and orbital periods of a few hours. When the outer layers of the companion overflow the "Roche lobe", the companion loses matter through the first Lagrangian point L_1 of the rotating binary system. When the white dwarf is only weakly magnetised, the matter forms an accretion disc around it and eventually reaches its surface. "Dwarf novae" (DN) are CVs that show outbursts lasting for about a week and separated by weeks to months of quiescence. U Gem is the prototype of dwarf novae. The brightness in the visible light of U Gem increases 100-fold every 120 days or so, and returns to the original level after a week or two. The DN phenomenon is due to a specific accretion disc limit-cycle instability, tidal torques, and fluctuations in the mass-transfer rate from the secondary. The geometry of accretion is very different in magnetic CVs, where accretion discs are either truncated or absent and accretion occurs along the magnetic field lines. There is a solid observational evidence for accretion discs in CVs based on very accurate photometry and spectroscopy. *[http://www.amazon.com/Cataclysmic-Variable-Stars-Cambridge-Astrophysics/dp/052154209X/ref=pd_sim_b_3/105-3740034-0846059 B. Warner, ''Cataclysmic Variable Stars'', 1995, 2003, Cambridge University Press] *[http://arxiv.org/abs/astro-ph/0102072 Lasota J.-P., 2001, ''The disc instability model of dwarf-novae and low-mass X-ray binary transients'', New Astron. Rev., '''45.7''', 449] *[http://astro.fit.edu/cv/fitdisk.html The accretion disk simulator by the cataclysmic variable group at The Florida Institute of Technology.] |
== Accretion discs in Quasars and other active galactic nuclei (AGN) ==
Most galaxies have supermassive (millions to billions of solar masses) black holes at their centres (nuclei). In AGN, the black hole accretion produces radiative power that usually outshines its host galaxy. The accretion disc is surrounded by a hot corona which contains clouds of gas. Fast moving clouds produce broad lines (BRL) and slow moving clouds produce narrow lines (NRL) in the AGN spectra. A large torus of gas and dust partially obscures the central part, which affects the observed appearance of an AGN, as Figure 4 explains.
| [[Image:AGN-scheme.jpg|frame|400px|center|AGN unification scheme. Green arrows indicate the AGN type that is seen from a certain viewing angle]] | Property | Quasars | Seyfert Galaxies | Radio Galaxies | Blazars |
|---|---|---|---|---|---|
| Galaxy type | Spiral, Elliptical | Spiral | Giant Elliptical | Elliptical | |
| Appearance | compact, blue | compact, bright nucleus | elliptical | bright, star-like | |
| Maximum luminosity | 100-1,000 Milky Way | comparable to bright Spirals | strong radio | 10,000 Milky Way | |
| Continuum spectrum | non-thermal | non-thermal | non-thermal | non-thermal | |
| Absorbtion lines | yes | none | yes | none | |
| Variability | days to weeks | days to weeks | days | hours | |
| Radio emission | some | weak | strong | weak | |
| Redshifts | z > 0.5 | z ~ 0.5 | z < 0.05 | z ~ 0.1 |
AGN are generally divided into two families, "radio loud" and "radio quiet", depending
on whether they exhibit jets or not. The viewing angle gives rise to several AGN types that are
distinguished by their emission properties. Among them, the spiral galaxies with
broad and narrow emission lines (Seyfert 2) or galaxies with just narrow emission lines
(Seyfert 1, where the dust torus obscures the BLR) and their counterparts in the radio loud
family, the broad line (BLRG viewing angle above ~60°) and narrow line radio galaxies
(NLRG viewing angle below ~60°) with jets and radio lobes perpendicular to the accretion
disc, as well as radio loud and radio quiet quasars (i.e. quasi-stellar objects).
The latter are the most luminous beacons in the universe and observed up to highest
redshifts, implying cosmological distance and gigantic energy output. Therefore, despite their name,
quasi-stellar objects are anything but stars. However, because quasars shine at such large
distances, it is not possible to resolve the bright core. Recent observations detect jets and
nebulosity around some of them.
*[http://press.princeton.edu/titles/6660.html J.H. Krolik, 1998, ''Active Galactic Nuclei: From the Central Black Hole to the Galactic Environment'', Princeton University Press]
*[http://www.astro.bas.bg/~petrov/galaxies_files/agn.html Online compilation by G.T.Petrov, 2004]
== Accretion discs in Microquasars and X-ray binaries ==
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[[Image:Mirabel-microquasar-quasar.gif |frame|400px|left| Microquasars found in several X-ray binaries in our Galaxy are scaled down versions of quasars, as pointed out by Felix Mirabel, who also coined the name "microquasar". This figure first appeared in several of Mirabel's articles.]] |
[[Image:x-ray-binaries-orosz.jpg|frame|400px|left| Black hole X-ray binaries in our Galaxy. The figure shows the companion star and the accretion disc drawn to scale. For a comparison, the Sun - Mercury distance is shown. (Figure by Jerome Arthur Orosz).]] |
Main-sequence secondary stars in orbit with accreting neutron stars or black holes (neutron star binaries or black hole binaries, respectively) are common objects in the Galaxy. Neutron stars are often magnetised, especially young ones, such that their accretion discs are disrupted by magnetic fields or do not exist at all. Matter in these cases is lead by partial or total column accretion to the compact object. In comparison to CVs their spectral energy distribution is observed up to the X-ray regime, since neutron stars and black holes have a much stronger gravitational potential. X-ray binaries are, depending on the mass of the companion star, roughly divided into two categories, the low-mass X-ray binaries, LMXBs (in figure 6, systems with coloured companion), and the high-mass X-ray binaries, HMXB (in figure 6, systems with white companion), where soft X-ray transients and X-ray pulsars are respective sub-classes. Soft X-ray transients with NSs or BHs show quasi-periodic outbursts. Many, if not all, black hole X-ray binaries exhibit in addition relativistic twin jets that propagate along the rotational axis of the compact object and are called microquasars.
*[http://adsabs.harvard.edu/abs/2003astro.ph..6213M J.E. McClintock and R.A. Remillard, 2003, ''Black Hole Binaries'']
== Accretion discs in gamma ray bursts (GRBs) ==
The most energetic explosions seen in the universe are gamma-ray bursts. They are short, collimated flares of low-energy \gamma-rays with relativistic emission simultaneously also at longer wavelengths (e.g., X-ray flashes, radio jets). Observations indicate that GRBs are cosmological and followed by slowly fading afterglows. The duration of GRB prompt emission can last from 0.01 - 2 seconds (short bursts) up to 2 - 500 seconds (long bursts) and may be explained by merging compact objects or failed supernovae (collapsars), respectively. Afterglows on the other hand are observed and monitored from a couple of days up to several years. All evidence on the origin of the inner engines (i.e., mergers, collapses, pulsars) of GRBs is deduced indirectly. Energetic requirements suggest, however, a similar configuration of the end products: the formation of a solar-mass black hole surrounded by a massive debris disc (~ 0.1 Msun) with a huge accretion rate. The time scale of the burst is determined by the accretion time of this disc. According to these time scales accretion discs in GRBs are most likely hyper-accreting. This means, the temperatures and densities at the required accretion rates are such, that neutrino production is switched on and the electrons are mildly relativistic and degenerate. Generally, GRBs seem to show similarities to radio-loud AGN and galactic microquasars, since all these systems eject strongly collimated, more or less relativistic flows of matter and involve accretion onto a black hole.
*[http://arxiv.org/abs/astro-ph/0405503 Piran T., 2005, "The Physics of Gamma-Ray Bursts", Rev.Mod.Phys., 76, 1143] *[http://lyra.berkeley.edu/grbox/grbox.php Gamma-Ray Burst Online Index]
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