Editing AU Microscopii

{{Short description|Star in the constellation Microscopium}}
{{Starbox begin
 | 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|09.53250}}<ref name=GaiaDR3/>
 | dec         = {{DEC|–31|20|27.2379}}<ref name=GaiaDR3/>
 | appmag_v    = 8.73<ref name=aaa460_3_695/>
 | constell    = [[Microscopium]]
}}
{{Starbox character
 | class       = M1Ve<ref name=aaa460_3_695/>
 | appmag_1_passband = V
 | appmag_1    = {{val|8.627|0.052}}<ref name="Donati2023"/>
 | appmag_2_passband = J
 | appmag_2    = {{val|5.436|0.017}}<ref name="Donati2023"/>
 | b-v         = 1.45
 | u-b         = 1.01
 | variable    = [[Flare star|Flare&nbsp;star]]
}}
{{Starbox astrometry
 | radial_v    = {{val|-6.90|0.37}}<ref name=GaiaDR3/>
 | prop_mo_ra  = +281.319
 | prop_mo_dec = -360.148
 | pm_footnote = <ref name=GaiaDR3/>
 | parallax    = 102.9432
 | p_error     = 0.0231
 | parallax_footnote = <ref name=GaiaDR3/>
 | absmag_v    = 8.61
}}
{{Starbox detail
 | radius      = {{val|0.82|0.02}}<ref name="Donati2023"/>
 | mass        = {{val|0.60|0.04}}<ref name="Donati2023"/>
 | luminosity  = {{val|0.102|0.002}}<ref name="Donati2023"/>
 | gravity     = {{val|4.52|0.05}}<ref name="Donati2023"/>
 | temperature = {{val|3665|31}}<ref name="Donati2023"/>
 | age_myr     = {{val|23|3}}, {{val|18.5|2.4}}<ref name="Donati2023"/>
 | rotation    = {{val|4.8367|0.0006|ul=d}}<ref name="Szabó2021"/>
 | rotational_velocity = {{val|8.5|0.2}}<ref name="Donati2023"/>
}}
{{Starbox catalog
| names = [[Cordoba Durchmusterung|CD]]&nbsp;-31°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
| NSTED=HD-197481
| ARICNS=01685
}}
{{Starbox end}}
'''AU Microscopii''' (AU Mic) is a young [[red dwarf]] [[star]] located {{Convert|31.7|ly|pc|abbr=off|lk=on}} away &ndash; about 8 times as far as the 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|β Pictoris]], AU Microscopii has a circumstellar disk of dust known as a [[debris disk]] and at least three [[exoplanet]]s, with the presence of an additional planet being likely.<ref name=Wittrock2023/><ref name="Donati2023"/>

==Stellar properties==
AU Mic is a young star at only 22 million years old; less than 1% of the age of the Sun.<ref name=PlavchanNature_2020/> With a [[stellar classification]] of M1&nbsp;Ve,<ref name=aaa460_3_695/> it is a [[red dwarf star]]<ref name=baas23_1382/> with a physical radius of 75% that of the [[Sun]]. Despite being 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 3,700&nbsp;[[Kelvin|K]], 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|β 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/>

[[File:AUMicLightCurve.png|thumb|left|A [[light curve]] for AU Microscopii, plotted from ''[[Transiting Exoplanet Survey Satellite|TESS]]'' data<ref name=MAST/>]]
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/>
{{clear left}}

== Planetary system ==
AU Microscopii's debris disk has an asymmetric structure and an inner gap or hole cleared of debris, which 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"/> However, in 2020 the discovery of a Neptune-sized planet was announced based on [[astronomical transit|transit]] observations by [[Transiting Exoplanet Survey Satellite|TESS]].<ref name=PlavchanNature_2020/> Its rotation axis is well aligned with the rotation axis of the parent star, with the misalignment being equal to 5{{±|16|15}}°.<ref name=Duncan2020/>

Since 2018, a second planet, AU Microscopii c, was suspected to exist. It was confirmed in December 2020, after additional transit events were documented by the TESS observatory.<ref name=Martioli2020/> A 2024 study which performed measurements of [[Rossiter–McLaughlin effect]] for the planet c revealed that the planet is possibly misaligned with the star's rotation axis, returning a poorly constrained value of projected [[Axial tilt#Extrasolar planets|obliquity]] ''λ''<sub>c</sub> = {{val|67.8|31.7|49.0|u=deg}}.<ref name=Yu2024 />

A third planet in the system was suspected since 2022 based on [[transit-timing variation]]s,<ref name=Wittrock2022/> and "validated" in 2023, although several possible orbital periods of planet d cannot be ruled out yet. This planet has a mass comparable to that of Earth.<ref name=Wittrock2023/> [[Doppler spectroscopy|Radial velocity]] observations have also found evidence for a fourth, outer planet as of 2023.<ref name="Donati2023"/> Observations of the AU Microscopii system with the [[James Webb Space Telescope]] were unable to confirm the presence of previously unknown companions.<ref name="Joshua E 2308">{{Cite journal |last1=Lawson |first1=Kellen |last2=Schlieder |first2=Joshua E. |last3=Leisenring |first3=Jarron M. |last4=Bogat |first4=Ell |last5=Beichman |first5=Charles A. |last6=Bryden |first6=Geoffrey |last7=Gáspár |first7=András |last8=Groff |first8=Tyler D. |last9=McElwain |first9=Michael W. |last10=Meyer |first10=Michael R. |last11=Barclay |first11=Thomas |last12=Calissendorff |first12=Per |last13=De Furio |first13=Matthew |last14=Ygouf |first14=Marie |last15=Boccaletti |first15=Anthony |date=2023-10-01 |title=JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii |journal=The Astronomical Journal |volume=166 |issue=4 |pages=150 |doi=10.3847/1538-3881/aced08 |doi-access=free |arxiv=2308.02486 |bibcode=2023AJ....166..150L |issn=0004-6256}}</ref> Observations with [[CHEOPS]] also detected strong TTVs of AU Mic c, which can be explained with planet d on a 12.6 day orbit. The mass of planet d is found to be only about 20% of the mass of earth (or two [[Mars]] masses) according to this study.<ref name="Boldog2025">{{Cite journal |arxiv=2501.09058 |last1=Matrà |first1=L. |title=REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths |date=2025-01-15 |last2=Marino |first2=S. |last3=Wilner |first3=D. J. |last4=Kennedy |first4=G. M. |last5=Booth |first5=M. |last6=Krivov |first6=A. V. |last7=Williams |first7=J. P. |last8=Hughes |first8=A. M. |last9=Burgo |first9=C. del|journal=Astronomy and Astrophysics |volume=693 |doi=10.1051/0004-6361/202451397 |bibcode=2025A&A...693A.151M }}</ref>

{{OrbitboxPlanet begin
| name = AU Microscopii
| table_ref = <ref name=Martioli2020/><ref name="Cale2021"/><ref name=Wittrock2023/><ref name="Donati2023"/><ref name="Boldog2025"/>
}}
{{OrbitboxPlanet
| exoplanet = b
| mass_earth = {{val|10.2|3.9|2.7}}
| radius_earth = {{val|4.07|0.17}}
| semimajor = {{val|0.0645|0.0013}}
| period = {{val|8.4630351|0.0000003}}
| eccentricity = {{val|0.00021|0.00006}}
| inclination = {{val|89.9904|0.0036|0.0019}}
}}
{{OrbitboxPlanet
| exoplanet = d
| mass_earth = {{val|1.014|0.146}} or<br />{{val|0.203|0.022|0.024}}
| radius_earth = 
| semimajor = 
| period = {{val|12.73812|0.00128}}
| eccentricity = {{val|0.00097|0.00042}}
| inclination = {{val|88.10|0.43}}
}}
{{OrbitboxPlanet
| exoplanet = c
| mass_earth = {{val|14.2|4.8|3.5}}
| radius_earth = {{val|3.24|0.16}}
| semimajor = {{val|0.1101|0.0020}}
| period = {{val|18.85901|0.00009}}
| eccentricity = {{val|0.01056|0.00089}}
| inclination = {{val|89.589|0.058|0.068}}
}}
{{OrbitboxPlanet hypothetical
| exoplanet = e
| mass_earth = {{val|35.2|6.7|5.4}}
| radius_earth = 
| semimajor = 
| period = {{val|33.39|0.10}}
| eccentricity = 
| inclination = 
}}
{{OrbitboxPlanet disk
| disk = Debris disk
| periapsis =<50
| apoapsis =>150
| inclination = <!--Inclination from the plane of the sky, in degrees-->
}}
{{Orbitbox end}}

===Debris disk===
[[Image:Debris disk AU Mic HST.jpg|left|thumb|[[Hubble Space Telescope]] image of the debris disk around AU Microscopii.]]
[[File:Mysterious ripples moving through the disc of AU Microscopii.webm|thumb|left|This short time lapse sequence shows images of the debris disk's "fast-moving features".]]

[[File:Dusty Debris Disk Around AU Mic (au-mic1).jpeg|thumb|left|300px|[[James Webb Space Telescope]] has imaged (Au Mic) the inner workings of a dusty disk surrounding a nearby red dwarf star.<ref>{{cite news |date=October 18, 2023 |title=Dusty Debris Disk Around AU Mic6 |url=https://esawebb.org/images/au-mic1/}}</ref> ]]

All-sky observations with the [[IRAS|Infrared Astronomy Satellite]] revealed faint infrared emission from AU Microscopii.<ref>{{Cite web |title=IRASFSC - IRAS Faint Source Catalog, Version 2.0 |url=https://heasarc.gsfc.nasa.gov/W3Browse/all/irasfsc.html |access-date=2024-05-10 |website=heasarc.gsfc.nasa.gov}}</ref><ref>{{Cite journal |last=Moshir |first=M. |display-authors=etal |date=1990-01-01 |title=IRAS Faint Source Catalogue, version 2.0. |url=https://ui.adsabs.harvard.edu/abs/1990IRASF.C......0M |journal=IRAS Faint Source Catalogue |pages=0|bibcode=1990IRASF.C......0M }}</ref> This emission is due to a circumstellar [[Debris disk|disk of dust]] which 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 at nearly 90 degrees,<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 |s2cid = 4406070}}</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" />  The debris disk is therefore referred to as "gas-poor", as the primordial gas within the circumstellar system has been mostly depleted.<ref>{{Cite journal |last1=Roberge |first1=Aki |last2=Weinberger |first2=Alycia J. |last3=Redfield |first3=Seth |last4=Feldman |first4=Paul D. |date=2005-06-01 |title=Rapid Dissipation of Primordial Gas from the AU Microscopii Debris Disk |url=https://ui.adsabs.harvard.edu/abs/2005ApJ...626L.105R |journal=The Astrophysical Journal |volume=626 |issue=2 |pages=L105–L108 |doi=10.1086/431899 |arxiv=astro-ph/0505302 |bibcode=2005ApJ...626L.105R |issn=0004-637X}}</ref>  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 have at least six lunar masses.<ref>{{cite journal|author1=C. H. Chen |author2=B. M. Patten |author3=M. W. Werner |author4=C. D. Dowell |author5=K. R. Stapelfeldt |author6=I. Song |author7=J. R. Stauffer |author8=M. Blaylock |author9=K. D. Gordon |author10=V. Krause  |name-list-style=amp |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|doi-access=free }}</ref>

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|author1=Michael C. Liu |author2=Brenda C. Matthews |author3=Jonathan P. Williams |author4=Paul G. Kalas  |name-list-style=amp |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 |s2cid=9178164 }}</ref> while scattered light images estimate the inner hole to be 12 AU in radius.<ref name="KIRSTETAL05" />  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" /> The inner part of the disk is [[asymmetry|asymmetric]] and shows structure in the inner 40 AU.<ref name="LIU04" />  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" /> The [[surface brightness]] (brightness per area) of the disk in the near infrared <math style="vertical-align:+0em">\scriptstyle I</math> as a function of projected distance <math style="vertical-align:+0em">\scriptstyle r</math> from the star follows a characteristic shape.  The inner <math style="vertical-align:+0em">\scriptstyle r\,<\,15 AU</math> of the disk appear approximately constant in density and the brightness is unchanging, more-or-less flat.<ref name="KIRSTETAL05" />  Around  <math style="vertical-align:-0.07em">\scriptstyle r\, \approx\, 15 AU</math> the density and surface brightness begins to decrease: first it decreases slowly in proportion to distance as <math style="vertical-align:+0em">\scriptstyle I\, \propto \,  r^{-1.8}</math>; then outside <math style="vertical-align:+0em">\scriptstyle r\, \approx\, 43 AU</math>, the density and brightness drops much more steeply, as <math style="vertical-align:+0em">\scriptstyle I\, \propto \, r^{-4.7}</math>.<ref name="KIRSTETAL05" />  This "broken power-law" shape is similar to the shape of the profile of β Pic's disk.

In October 2015 it was reported that astronomers using the [[Very Large Telescope]] (VLT) had detected very unusual outward-moving features in the disk. By comparing the VLT images with those taken by the [[Hubble Space Telescope]] in 2010 and 2011 it was found that the wave-like structures are moving away from the star at speeds of up to 10 kilometers per second (22,000 miles per hour). The waves farther away from the star seem to be moving faster than those close to it, and at least three of the features are moving fast enough to escape the gravitational pull of the star.<ref name="Ripples">{{cite web|title=Mysterious Ripples Found Racing Through Planet-Forming Disk |url=http://hubblesite.org/newscenter/archive/releases/2015/36/ |website=Hubblesite |access-date=8 October 2015 |archive-url=https://web.archive.org/web/20151011023230/http://hubblesite.org/newscenter/archive/releases/2015/36/full/ |archive-date=11 October 2015 |url-status=live }}</ref> Follow-up observations with the [[VLT-SPHERE|SPHERE]] instrument on the [[Very Large Telescope]] were able to confirm the presence of the fast-moving features,<ref>{{Cite journal |last1=Boccaletti |first1=A. |last2=Sezestre |first2=E. |last3=Lagrange |first3=A.-M. |last4=Thébault |first4=P. |last5=Gratton |first5=R. |last6=Langlois |first6=M. |last7=Thalmann |first7=C. |last8=Janson |first8=M. |last9=Delorme |first9=P. |last10=Augereau |first10=J.-C. |last11=Schneider |first11=G. |last12=Milli |first12=J. |last13=Grady |first13=C. |last14=Debes |first14=J. |last15=Kral |first15=Q. |date=2018-06-01 |title=Observations of fast-moving features in the debris disk of AU Mic on a three-year timescale: Confirmation and new discoveries |url=https://www.aanda.org/articles/aa/abs/2018/06/aa32462-17/aa32462-17.html |journal=Astronomy & Astrophysics |language=en |volume=614 |pages=A52 |doi=10.1051/0004-6361/201732462 |arxiv=1803.05354 |bibcode=2018A&A...614A..52B |issn=0004-6361}}</ref> and James Webb Space Telescope observations found similar features within the disk in two NIRCam filters;<ref name="Joshua E 2308"/> however, these features have not been detected in the radio with [[Atacama Large Millimeter Array]] observations.<ref>{{Cite journal |last1=Daley |first1=Cail |last2=Hughes |first2=A. Meredith |last3=Carter |first3=Evan S. |last4=Flaherty |first4=Kevin |last5=Lambros |first5=Zachary |last6=Pan |first6=Margaret |last7=Schlichting |first7=Hilke |last8=Chiang |first8=Eugene |last9=Wyatt |first9=Mark |last10=Wilner |first10=David |last11=Andrews |first11=Sean |last12=Carpenter |first12=John |date=2019-04-01 |title=The Mass of Stirring Bodies in the AU Mic Debris Disk Inferred from Resolved Vertical Structure |journal=The Astrophysical Journal |volume=875 |issue=2 |pages=87 |doi=10.3847/1538-4357/ab1074 |doi-access=free |arxiv=1904.00027 |bibcode=2019ApJ...875...87D |issn=0004-637X}}</ref><ref name="Evan S 2207">{{Cite journal |last1=Vizgan |first1=David |last2=Meredith Hughes |first2=A. |last3=Carter |first3=Evan S. |last4=Flaherty |first4=Kevin M. |last5=Pan |first5=Margaret |last6=Chiang |first6=Eugene |last7=Schlichting |first7=Hilke |last8=Wilner |first8=David J. |last9=Andrews |first9=Sean M. |last10=Carpenter |first10=John M. |last11=Moór |first11=Attila |last12=MacGregor |first12=Meredith A. |date=2022-08-01 |title=Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade |journal=The Astrophysical Journal |volume=935 |issue=2 |pages=131 |doi=10.3847/1538-4357/ac80b8 |doi-access=free |arxiv=2207.05277 |bibcode=2022ApJ...935..131V |issn=0004-637X}}</ref> These fast-moving features have been described as "dust avalanches", where dust particles catastrophically collide into planetesimals within the disk.<ref>{{Cite journal |last1=Chiang |first1=Eugene |last2=Fung |first2=Jeffrey |date=2017-10-05 |title=Stellar Winds and Dust Avalanches in the AU Mic Debris Disk |journal=The Astrophysical Journal |volume=848 |issue=1 |pages=4 |doi=10.3847/1538-4357/aa89e6 |doi-access=free |arxiv=1707.08970 |bibcode=2017ApJ...848....4C |issn=0004-637X}}</ref><ref name="Evan S 2207"/>

==Methods of observation==
[[File:Hubble captures blobs of material sweeping through stellar disc AU Microscopii.tif|thumb|Hubble observations of blobs of material sweeping through stellar disc.<ref>{{cite web |title=Hubble captures blobs of material sweeping through stellar disc |url=https://www.spacetelescope.org/images/opo1902a/ |website=www.spacetelescope.org |access-date=10 January 2019 |language=en}}</ref>]]
AU Mic's disk has been observed at a variety of different [[wavelength]]s, giving humans 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 Earth's 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 humans 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 | access-date=2007-01-11 | archive-url= https://web.archive.org/web/20070115065231/http://www.berkeley.edu/news/media/releases/2007/01/08_dust.shtml| archive-date= 15 January 2007 | url-status= live}}</ref>

{{CSS image crop|Image=The 74 exocomet belts imaged by ALMA’s REASONS survey, showing belts of all shapes, sizes and ages (REASONS comboplot full nonames).jpg|bSize=1600|cWidth=160|cHeight=160|oTop=960|oLeft=800|Location=right|Description=millimeter observation of the disk from the REASONS survey<ref name="Martrá2025"/>}}

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 with the [[James Clerk Maxwell Telescope]], [[Spitzer Space Telescope]], and the [[James Webb Space Telescope]]. 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.  
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== Gallery ==
<gallery>
Image:The View from Within AU Microscopii's Disk.jpg|Artist's impression of AU Microscopii Credit: NASA/ESA/G. Bacon (STScI)
File:Hubble sees evaporating planet getting the hiccups (opo2315a).jpg|Artist's impression of AU Microscopii and planet AU Mic b, which is loosing mass.
</gallery>

== See also ==

* [[List of exoplanets discovered in 2020]] - AU Microscopii b and c
* [[List of exoplanets discovered in 2023]] - AU Microscopii d

== References ==
{{reflist|30em|refs=

<ref name="Martrá2025">{{Cite arxiv |eprint=2501.09058 |class=astro-ph |last=Matrà |first=L. |title=REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths |date=2025-01-15 |last2=Marino |first2=S. |last3=Wilner |first3=D. J. |last4=Kennedy |first4=G. M. |last5=Booth |first5=M. |last6=Krivov |first6=A. V. |last7=Williams |first7=J. P. |last8=Hughes |first8=A. M. |last9=Burgo |first9=C. del}}</ref>

<ref name=GaiaDR3>{{Cite Gaia DR3|6794047652729201024}}</ref>

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}}

==External links==
{{commons category}}
* {{cite web
| year=2004
| url = http://www.solstation.com/stars/au-mic3.htm
| title = AU and AT Microscopii AB
| publisher = SolStation
| access-date = 2006-12-20
| archive-url= https://web.archive.org/web/20061111100248/http://solstation.com/stars/au-mic3.htm| archive-date= 11 November 2006 | url-status= live}}

{{Stars of Microscopium}}

{{DEFAULTSORT:AU Microscopii}}
[[Category:Microscopium]]
[[Category:M-type main-sequence stars]]
[[Category:Flare stars]]
[[Category:Circumstellar disks]]
[[Category:Objects with variable star designations|Microscopii, AU]]
[[Category:Henry Draper Catalogue objects|197481]]
[[Category:Articles containing video clips]]
[[Category:Gliese and GJ objects|0803]]
[[Category:Hipparcos objects|102409]]
[[Category:Durchmusterung objects]]
[[Category:Planetary systems with two confirmed planets]]
[[Category:Beta Pictoris moving group]]