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{{Starbox begin
== largescale production. Timberland Shoes Usa ==
| name = AU Microscopii
}}
{{Starbox image
| image = [[Image:HD197481 2MASS JBAND.png|250px]]
| caption = AU Microscopii, J band image, [[2MASS]].
}}
{{Starbox observe
| epoch      = J2000
| ra          = {{RA|20|45|09.53147}}<ref name=aaa474_2_653/>
| dec        = {{DEC|–31|20|27.2425}}<ref name=aaa474_2_653/>
| appmag_v    = 8.73<ref name=aaa460_3_695/>
| constell    = [[Microscopium]]
}}
{{Starbox character
| class      = M1&nbsp;Ve<ref name=aaa460_3_695/>
| b-v        = 1.45
| u-b        = 1.01
| variable    = [[Flare star|Flare&nbsp;star]]
}}
{{Starbox astrometry
| radial_v    = –6.0<ref name=aaa460_3_695/>
| prop_mo_ra  = +279.96<ref name=aaa474_2_653/>
| prop_mo_dec = -360.61<ref name=aaa474_2_653/>
| parallax    = 100.91
| p_error    = 1.06
| parallax_footnote = <ref name=aaa474_2_653/>
| absmag_v    = 8.61
}}
{{Starbox detail
| radius      = 0.84<ref name=apj698_2_1068/>
| mass        = 0.31<ref name=apj698_2_1068/>
| luminosity  = 0.09<ref name=apj698_2_1068/>
| temperature = 3,500 ± 100<ref name=apj698_2_1068/>
| age_myr    = 12 ± 2<ref name=apj698_2_1068/>
| rotational_velocity = 9.3<ref name=aaa460_3_695/>
}}
{{Starbox catalog
| names = [[Cordoba Durchmusterung|CD]]&nbsp;-31&deg;17815, [[General Catalogue of Trigonometric Parallaxes|GCTP]]&nbsp;4939.00, [[Gliese-Jahreiss catalogue|GJ]]&nbsp;803, [[Henry Draper catalogue|HD]]&nbsp;197481, [[Hipparcos catalogue|HIP]]&nbsp;102409, [[Luyten Two-Tenths catalogue|LTT]]&nbsp;8214, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;212402, Vys&nbsp;824, LDS&nbsp;720&nbsp;A.
}}
{{Starbox reference
| Simbad=AU+Microscopii
| ARICNS=01685
}}
{{Starbox end}}
'''AU Microscopii''' (AU Mic) is a small [[star]] located {{Convert|32.3|ly|pc|abbr=off|lk=on}} away &ndash; about 8 times as far as our closest star after the [[Sun]].<ref name="KALASETAL04"/> The [[apparent visual magnitude]] of AU Microscopii is 8.73,<ref name=aaa460_3_695/> which is too dim to be seen with the naked eye. It was given this [[Variable star designation|designation]] because it is in the southern constellation [[Microscopium]] and is a [[variable star]]. Like [[Beta Pictoris|&beta; Pictoris]], AU Microscopii has a circumstellar disk of dust known as a [[debris disk]].


==Stellar properties==
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AU Mic is a young star at only 12 million years old; less than 1% of the age of the [[Sun]].<ref name="PLAVCHANETAL05"/> With a [[stellar classification]] of M1&nbsp;Ve,<ref name=aaa460_3_695/> it is [[red dwarf star]]<ref name=baas23_1382/> with a physical radius of 60% that of the [[Sun]]. Despite being more than half the Sun's mass,<ref name="DELZANNA2002"/><ref name=sci303_5666_1982/> it is radiating only 9%<ref name=apj698_2_1068/> as much luminosity as the Sun. This energy is being emitted from the star's [[stellar atmosphere|outer atmosphere]] at an [[effective temperature]] of 3,730&nbsp;[[Kelvin|K]],<ref name = "LINSKYETAL82"/> giving it the cool orange-red hued glow of an [[M-type star]].<ref name=csiro/> AU Microscopii is a member of the [[Beta Pictoris Moving Group|&beta; Pictoris moving group]].<ref name=araa41_1_685/><ref name=apj520_2_L123/> AU Microscopii may be [[gravitationally bound]] to the binary star system [[AT Microscopii]].<ref name=aaa302_193/>
 
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AU Microscopii has been observed in every part of the [[electromagnetic spectrum]] from [[radio]] to [[X-ray]] and is known to undergo [[flare star|flaring]] activity at all these wavelengths.<ref name=apj421_2_800/><ref name=apj414_2_L49/><ref name=apj312_822/><ref name = "TSIKOUDI2000"/> Its flaring behaviour was first identified in 1973.<ref name=apjs25_1/><ref name=mnras197_815/> 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 [[UBV photometric system|V band]] brightness variation was approximately 0.3 [[Absolute magnitude|magnitude]]s in 1971; by 1980 it was merely 0.1 magnitudes.<ref name=aaa174_1_139/>
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==Debris disk==
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[[Image:Debris disk AU Mic HST.jpg|left|thumb|[[Hubble Space Telescope]] image of the debris disk around AU Microscopii]]
 
AU Microscopii harbors its own disk of dust, first resolved at optical wavelengths in 2003 by [[Paul Kalas]] and collaborators using the [[UH88|University of Hawaii 2.2-m telescope]] on [[Mauna Kea]], Hawaii.<ref name = "KALASETAL04" /> This large debris disk faces the earth edge-on,<ref>{{cite journal|author = Paul Kalas, James R. Graham and Mark Clampin|title = A planetary system as the origin of structure in Fomalhaut's dust belt|journal = Nature|date = 23 June 2005|pages = 1067–1070|bibcode = 2005Natur.435.1067K|doi = 10.1038/nature03601|issue = 7045|volume = 435|pmid = 15973402|arxiv = astro-ph/0506574 }}</ref> and measures at least 200 [[Astronomical unit|AU]] in radius. At these large distances from the star, the lifetime of dust in the disk exceeds the age of AU Microscopii.<ref name = "KALASETAL04" />  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.<ref name = "ROBERGEETAL05">{{cite journal|author = Aki Roberge, Alycia J. Weinberger, Seth Redfield, and Paul D. Feldman|title = Rapid Dissipation of Primordial Gas from the AU Microscopii Debris Disk|journal = The Astrophysical Journal|date = 20 June 2005|volume = 626|issue = 2|pages = L105–L108|bibcode =2005ApJ...626L.105R|doi = 10.1086/431899|arxiv = astro-ph/0505302 }}</ref>  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 [[planetesimal]]s from which the dust is produced are inferred to has at least six lunar masses.<ref>{{cite journal|author = C. H. Chen, B. M. Patten, M. W. Werner, C. D. Dowell, K. R. Stapelfeldt, I. Song, J. R. Stauffer, M. Blaylock, K. D. Gordon, and V. Krause|title = A Spitzer Study of Dusty Disks around Nearby, Young Stars|journal = The Astrophysical Journal|date = December 1, 2005|issue = 2|pages = 1372–1384|bibcode = 2005ApJ...634.1372C|doi = 10.1086/497124|volume = 634}}</ref>
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The [[Astronomical spectroscopy|spectral energy distribution]] of AU Microscopii's debris disk at [[Submillimetre astronomy|submillimetre]] wavelengths indicate the presence of an inner hole in the disk extending to 17 AU,<ref>{{cite journal|title = A Submillimeter Search of Nearby Young Stars for Cold Dust: Discovery of Debris Disks around Two Low-Mass Stars|author = Michael C. Liu, Brenda C. Matthews, Jonathan P. Williams, and Paul G. Kalas|journal = [[The Astrophysical Journal]]|date = June 10, 2004|volume = 608|issue = 1|pages = 526–532|bibcode = 2004ApJ...608..526L|doi = 10.1086/392531|arxiv = astro-ph/0403131 }}</ref> while scattered light images estimate the inner hole to be 12 AU in radius.<ref name = "KIRSTETAL05">{{cite journal|author = John E. Kirst, D. R. Ardila, D. A. Golimowski, M. Clampin, H. C. Ford, G. D. Illingworth, G. F. Hartig, F. Bartko, N. Benítez, J. P. Blakeslee, R. J. Bouwens, L. D. Bradley, T. J. Broadhurst, R. A. Brown, C. J. Burrows, E. S. Cheng, N. J. G. Cross, R. Demarco, P. D. Feldman, M. Franx, T. Goto, C. Gronwall, B. Holden, N. Homeier, L. Infante, R. A. Kimble, M. P. Lesser, A. R. Martel, S. Mei, F. Mennanteau, G. R. Meurer, G. K. Miley, V. Motta, M. Postman, P. Rosati, M. Sirianni, W. B. Sparks, H. D. Tran, Z. I. Tsvetanov, R. L. White, AND W. Zheng|title = Hubble Space Telescope Advanced Camera for Surveys Coronagraphic Imaging of the AU Microscopii Debris Disk|date=February 2005|journal = The Astronomical Journal|volume = 129|issue = 2|pages = 1008–1017|bibcode = 2005AJ....129.1008K|doi = 10.1086/426755}}</ref>  Combining the spectral energy distribution with the surface brightness profile yields a smaller estimate of the radius of the inner hole, 1 - 10 AU.<ref name = "METCHEVETAL05">{{cite journal|author = Stanimir A. Metchev, Joshua A. Eisner, and Lynne A. Hillenbrand|title = Adaptive Optics Imaging of the AU Microscopii Circumstellar Disk: Evidence for Dynamical Evolution|journal = The Astrophysical Journal|date = March 20, 2005|volume = 622|issue = 1|pages = 451–462|bibcode = 2005ApJ...622..451M|doi = 10.1086/427869|arxiv = astro-ph/0412143 }}</ref>
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The inner part of the disk is [[asymmetry|asymmetric]] and shows structure in the inner 40 AU.<ref name = "LIU04">{{cite journal|title = Substructure in the Circumstellar Disk Around the Young Star AU Microscopii|author = Michael C. Liu|journal = Science|date = 3 September 2004|volume = 305|pages = 1442–1444|url = http://www.sciencemag.org/cgi/content/full/305/5689/1442|doi = 10.1126/science.1102929|pmid = 15308766|issue = 5689|arxiv = astro-ph/0408164 |bibcode = 2004Sci...305.1442L }}</ref>  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.<ref name = "LIU04"/>
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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.<ref name = "METCHEVETAL05" /><ref name = "MASCIADRIETAL05">{{cite journal|author = E. Masciadri, R. Mundt, Th. Henning, and C. Alvarez|title = A Search for Hot Massive Extrasolar Planets around Nearby Young Stars with the Adaptive Optics System NACO|journal = The Astrophysical Journal|date = 1 June 2005|volume = 625|issue = 2|pages = 1004–1018|bibcode = 2005ApJ...625.1004M|doi = 10.1086/429687|arxiv = astro-ph/0502376 }}</ref>
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The surface brightness (brightness per area) of the disk as a function of projected distance <math>b</math> from the star follows a characteristic shape. The inner 15 AU of the disk appear approximately constant in density.<ref name = "KIRSTETAL05" />  Around <math>b \approx 15 AU</math> the density begins to decrease: first it decreases slowly as <math>b^{-\alpha}</math> where <math>\alpha \approx 1.8</math>; then outside <math>b \approx 43 AU</math>, the brightness drops more steeply, as <math>b^{-\alpha}</math> where <math>\alpha \approx 4.8</math>.<ref name = "KIRSTETAL05" />  This "broken power-law" shape is similar to the shape of the profile of β Pic's disk.
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[[Image:Hypothetical terrestrial planet and moon orbiting the red dwarf star AU Microscopii.jpg|right|thumb|Artist's impression of AU Microscopii Credit: NASA/ESA/G. Bacon (STScI)]]
 
AU Mic's disk has been observed at a variety of different [[wavelength]]s, giving us different types of information about the system. The light from the disk observed at [[visible light|optical wavelengths]] is stellar light that has reflected (scattered) off dust particles into our line of sight. Observations at these wavelengths utilize a [[coronagraph|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.<ref name="ucbn0108">{{cite news | first=Robert | last=Sanders | title=Dust around nearby star like powder snow | publisher=UC Berkeley News | date=2007-01-08 | url=http://www.berkeley.edu/news/media/releases/2007/01/08_dust.shtml | accessdate=2007-01-11 | archiveurl= http://web.archive.org/web/20070115065231/http://www.berkeley.edu/news/media/releases/2007/01/08_dust.shtml| archivedate= 15 January 2007 <!--DASHBot-->| deadurl= no}}</ref>
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Optical observations have been made with the [[Hubble Space Telescope]] and [[Keck Telescope]]s.  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]].
  <li>[http://www.vitrinaweb.es/index.php?page=item&id=105723 http://www.vitrinaweb.es/index.php?page=item&id=105723]</li>
 
 
==References==
  <li>[http://www.yqxysd.com/forum.php?mod=viewthread&tid=63038 http://www.yqxysd.com/forum.php?mod=viewthread&tid=63038]</li>
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}}
 
==External links==
* {{cite web
| year=2004
| url = http://www.solstation.com/stars/au-mic3.htm
| title = AU and AT Microscopii AB
| publisher = SolStation
| accessdate = 2006-12-20
| archiveurl= http://web.archive.org/web/20061111100248/http://solstation.com/stars/au-mic3.htm| archivedate= 11 November 2006 <!--DASHBot-->| deadurl= no}}
{{Nearest star systems|7}}
 
{{Stars of Microscopium}}
 
[[Category:Microscopium (constellation)]]
[[Category:M-type main-sequence stars]]
[[Category:Circumstellar disks]]
[[Category:Objects named with variable star designations|Microscopii, AU]]
[[Category:Henry Draper Catalogue objects|197481]]

Latest revision as of 22:30, 19 September 2014

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