AU Microscopii, J band image, 2MASS.
Epoch J2000 Equinox J2000
|Right ascension||20h 45m 09.53147s|
|Declination||–31° 20′ 27.2425″|
|Apparent magnitude (V)||8.73|
|Spectral type||M1 Ve|
|U−B color index||1.01|
|B−V color index||1.45|
|Variable type||Flare star|
|Radial velocity (Rv)||–6.0 km/s|
|Proper motion (μ)||RA: +279.96 mas/yr
Dec.: -360.61 mas/yr
|Parallax (π)||100.91 ± 1.06 mas|
|Distance||32.3 ± 0.3 ly
(9.9 ± 0.1 pc)
|Absolute magnitude (MV)||8.61|
|Temperature||3,500 ± 100 K|
|Rotational velocity (v sin i)||9.3 km/s|
|Age||12 ± 2 Myr|
AU Microscopii (AU Mic) is a small star located 32.3 light-years (9.9 parsecs) away – about 8 times as far as our 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.
AU Mic is a young star at only 12 million years old; less than 1% of the age of the Sun. With a stellar classification of M1 Ve, it is red dwarf star with a physical radius of 60% that of the Sun. Despite being more than half the Sun's mass, it is radiating only 9% as much luminosity as the Sun. This energy is being emitted from the star's outer atmosphere at an effective temperature of 3,730 K, giving it the cool orange-red hued glow of an M-type star. AU Microscopii is a member of the β Pictoris moving group. AU Microscopii may be gravitationally bound to the binary star system AT Microscopii.
AU Microscopii has been observed in every part of the electromagnetic spectrum from radio to X-ray and is known to undergo flaring activity at all these wavelengths. Its flaring behaviour was first identified in 1973. Underlying these random outbreaks is a nearly sinusoidal variation in its brightness with a period of 4.865 days. The amplitude of this variation changes slowly with time. The V band brightness variation was approximately 0.3 magnitudes in 1971; by 1980 it was merely 0.1 magnitudes.
AU Microscopii harbors its own disk of dust, first resolved at optical wavelengths in 2003 by Paul Kalas and collaborators using the University of Hawaii 2.2-m telescope on Mauna Kea, Hawaii. This large debris disk faces the earth edge-on, and measures at least 200 AU in radius. At these large distances from the star, the lifetime of dust in the disk exceeds the age of AU Microscopii. The disk has a gas to dust mass ratio of no more than 6:1, much lower than the usually assumed primordial value of 100:1. The debris disk is therefore referred to as "gas-poor". The total amount of dust visible in the disk is estimated to be at least a lunar mass, while the larger planetesimals from which the dust is produced are inferred to has at least six lunar masses.
The spectral energy distribution of AU Microscopii's debris disk at submillimetre wavelengths indicate the presence of an inner hole in the disk extending to 17 AU, while scattered light images estimate the inner hole to be 12 AU in radius. Combining the spectral energy distribution with the surface brightness profile yields a smaller estimate of the radius of the inner hole, 1 - 10 AU.
The inner part of the disk is asymmetric and shows structure in the inner 40 AU. The inner structure has been compared with that expected to be seen if the disk is influenced by larger bodies or has undergone recent planet formation.
The presence of the inner hole and asymmetric structure has led a number of astronomers to search for planets orbiting AU Microscopii. By 2007, no searches had led to any detections of planets.
The surface brightness (brightness per area) of the disk as a function of projected distance from the star follows a characteristic shape. The inner 15 AU of the disk appear approximately constant in density. Around the density begins to decrease: first it decreases slowly as where ; then outside , the brightness drops more steeply, as where . This "broken power-law" shape is similar to the shape of the profile of β Pic's disk.
(in order from star)
|Dust disk||<50–>150 AU||—||—|
Methods of observation
AU Mic's disk has been observed at a variety of different wavelengths, giving us different types of information about the system. The light from the disk observed at optical wavelengths is stellar light that has reflected (scattered) off dust particles into our line of sight. Observations at these wavelengths utilize a coronagraphic spot to block the bright light coming directly from the star. Such observations provide high-resolution images of the disk. Because light having a wavelength longer than the size of a dust grain is scattered only poorly, comparing images at different wavelengths (visible and near-infrared, for example) gives us information about the sizes of the dust grains in the disk.
Optical observations have been made with the Hubble Space Telescope and Keck Telescopes. The system has also been observed at infrared and sub-millimeter wavelengths. This light is emitted directly by dust grains as a result of their internal heat (modified blackbody radiation). The disk cannot be resolved at these wavelengths, so such observations are measurements of the amount of light coming from the entire system. Observations at increasingly longer wavelengths give information about dust particles of larger sizes and at larger distances from the star. These observations have been made with the James Clerk Maxwell Telescope and Spitzer Space Telescope.
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