MWC 480

Last updated
MWC 480
MWC480LightCurve.png
A visual band light curve for MWC 480, plotted from ASAS-SN data [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Auriga
Right ascension 04h 58m 46.2654s [2]
Declination +29° 50′ 36.990″ [2]
Apparent magnitude  (V)7.62 [3]
Characteristics
Spectral type A3psh3+ [4]
Astrometry
Proper motion (μ)RA: 4.793 [2]   mas/yr
Dec.: -25.348 [2]   mas/yr
Parallax (π)6.1815 ± 0.0761  mas [2]
Distance 528 ± 6  ly
(162 ± 2  pc)
Details
Mass 1.7-2.3 [5]   M☉
Radius 1.67 [4]   R☉
Luminosity 11.2 [4]   L☉
Temperature 8250 [3]   K
Rotational velocity (v sin i)102.0 ± 5.0 [6]  km/s
Age 6–7.1 [5]   Myr
Other designations
BD+29 774, HD  31648, HIP  23143, SAO  76866, GSC  01844-00503, 2MASS J04584626+2950370 [7]
Database references
SIMBAD data

MWC 480 is a single [4] star, about 500 light-years away in the constellation of Auriga. It is located in the Taurus-Auriga Star-Forming Region. [8] The name refers to the Mount Wilson Catalog of B and A stars with bright hydrogen lines in their spectra. [9] With an apparent magnitude of 7.62, [3] it is too faint to be seen with the naked eye.

Contents

Properties

Artist impression of the protoplanetary disc surrounding MWC 480.

MWC 480 is a young Herbig Ae/Be star, a class of young stars with spectral types of A or B, but are quite young and are still not main-sequence stars. MWC 480 is about 7 million years old. [5] It is about twice the mass of the Sun, [5] and is estimated to be about 1.67 solar radii. [4]

MWC 480 has X-ray emissions typical of a pre-main-sequence Herbig Ae/Be star but with an order of magnitude more photoelectric absorption. [4] It has a gas-dust envelope and is surrounded by a protoplanetary disc that is about 11% the mass of the Sun. [5] The disc is inclined about 37° towards the line of sight, on a position angle of about 148°. [5] Astronomers using the ALMA (Atacama Large Millimeter/submillimeter Array) have found that the protoplanetary disc surrounding MWC 480 contains large amounts of methyl cyanide (CH3CN), a complex carbon-based molecule. [10] Hydrogen cyanide (HCN) has also been detected in the disc. [11] No signs of planet formation have yet been detected.

Planetary system

In 2021, an imaging of the gas flows in the circumstellar disk has suggested a presence of shrouded Jupiter-mass planet about 245 AU from the star. [12]

Related Research Articles

<span class="mw-page-title-main">HD 100546</span> Star in the constellation Musca

HD 100546, also known as KR Muscae, is a pre-main sequence star of spectral type B8 to A0 located 353 light-years from Earth in the southern constellation of Musca. The star is surrounded by a circumstellar disk from a distance of 0.2 to 4 AU, and again from 13 AU out to a few hundred AU, with evidence for a protoplanet forming at a distance of around 47 AU.

HD 97048 or CU Chamaeleontis is a Herbig Ae/Be star 603 ly away in the constellation Chamaeleon. It is a variable star embedded in a dust cloud containing a stellar nursery, and is itself surrounded by a dust disk.

<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">AB Aurigae</span> Star in the constellation Auriga

AB Aurigae is a young Herbig Ae star in the Auriga constellation. It is located at a distance of approximately 531 light years from the Sun based on stellar parallax. This pre-main-sequence star has a stellar classification of A0Ve, matching an A-type main-sequence star with emission lines in the spectrum. It has 2.4 times the mass of the Sun and is radiating 38 times the Sun's luminosity from its photosphere at an effective temperature of 9,772 K. The radio emission from the system suggests the presence of a thermal jet originating from the star with a velocity of 300 km s−1. This is causing an estimated mass loss of 1.7×10−8 M☉ yr−1.

<span class="mw-page-title-main">HD 142527</span> Young star in the constellation of Lupus

HD 142527 is a binary star system in the constellation of Lupus. The primary star belongs to the Herbig Ae/Be star class, while the companion, discovered in 2012, is a red dwarf star or accreting protoplanet with a projected separation of less than 0.1″. The system is notable for its circumbinary protoplanetary disk and its discovery has helped refine models of planet formation. The orbit of companion is strongly inclined to the circumbinary protoplanetary disk.

SAO 206462 is a young binary star, surrounded by a circumstellar disc of gas and clearly defined spiral arms. It is situated about 440 light-years away from Earth in the constellation Lupus. The presence of these spiral arms seems to be related to the existence of planets inside the disk of gas surrounding the star. The disk's diameter is about twice the size of the orbit of Pluto.

<span class="mw-page-title-main">HD 259431</span> Young stellar object in the constellation Monoceros

HD 259431 is a young stellar object in the constellation of Monoceros.

<span class="mw-page-title-main">HD 169142</span> Pre-main-sequence star in the constellation Sagittarius

HD 169142 is a single Herbig Ae/Be star. Its surface temperature is 7650±150 K. HD 169142 is depleted of heavy elements compared to the Sun, with a metallicity Fe/H index of −0.375±0.125, but is much younger at an age of 7.5±4.5 million years. The star is rotating slowly and has relatively low stellar activity for a Herbig Ae/Be star.

<span class="mw-page-title-main">LkCa 15</span> Star system in the constellation Taurus

LkCa 15 is a T Tauri star in the Taurus Molecular Cloud. These types of stars are relatively young pre-main-sequence stars that show irregular variations in brightness. It has a mass that is about 97% of the Sun, an effective temperature of 4370 K, and is slightly cooler than the Sun. Its apparent magnitude is 11.91, meaning it is not visible to the naked eye.

<span class="mw-page-title-main">HD 36112</span> Star in the constellation Taurus

HD 36112, also known as MWC 758, is a young Herbig Ae star located in the constellation Taurus, surrounded by irregular rings of cosmic dust. The system is about 3.5 million years old. The disk has a cavity at 50 astronomical units and two spiral arms at 30-75 au that are seen in near-infrared scattered light, but only one spiral arm is seen in ALMA images.

<span class="mw-page-title-main">AK Scorpii</span> Binary star in the constellation Scorpius

AK Scorpii is a Herbig Ae/Be star and spectroscopic binary star about 459 light-years distant in the constellation Scorpius. The star belongs to the nearby Upper Centaurus–Lupus star-forming region and the star is actively accreting material. The binary is surrounded by a circumbinary disk that was imaged with VLT/SPHERE in scattered light and with ALMA.

<span class="mw-page-title-main">RY Tauri</span> Star in the constellation Taurus

RY Tauri is a young T Tauri star in the constellation of Taurus about 450 light years away, belonging to the Taurus Molecular Cloud. It is more massive than typical T Tauri stars, and may be an intermediate between this class and the Herbig Ae/Be star type.

HD 155448 is a quintuple star system consisting of 5 young B-type stars. With an apparent magnitude of 8.72, it is too dim to be visible with the naked eye.

<span class="mw-page-title-main">HK Tauri</span> Young binary star system in the constellation of Taurus

HK Tauri is a young binary star system in the constellation of Taurus about 434 light-years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">HD 150193</span> Young binary star system in the constellation Ophiuchus

HD 150193 is a binary star system in the constellation of Ophiuchus. The primary star was identified as a Herbig Ae/Be star with a strong solar wind, losing approximately a tenth of solar mass per million years. It does host a very small debris disk, likely due to disk truncation by the nearby stellar companion. The disk is inclined 38±9° to the plane of sky. It appears to be highly evolved and asymmetric, with indications of flattening and grains growth.

<span class="mw-page-title-main">DL Tauri</span> Protostar system with planetary system in the constellation of Taurus

DL Tauri is a young T Tauri-type pre-main sequence stars in the constellation of Taurus about 522 light years away, belonging to the Taurus Molecular Cloud. It is partially obscured by the foreground gas cloud rich in carbon monoxide, and is still accreting mass, producing 0.14 L☉ due to release of accretion energy. The stellar spectrum shows the lines of ionized oxygen, nitrogen, sulfur and iron.

<span class="mw-page-title-main">BF Orionis</span> Young protostar system

BF Orionis is a young Herbig Ae/Be star in the constellation of Orion about 1250 light years away, within the Orion Nebula. It is the most massive star of the small birth cluster of four stars.

<span class="mw-page-title-main">HD 100453</span> Young binary in constellation Centaurus

HD 100453 is a binary star system which lies in the constellation Centaurus about 350 light years away from the Sun and is a member of the open cluster Scorpius–Centaurus association.

<span class="mw-page-title-main">CQ Tauri</span> Star in the constellation Taurus

CQ Tauri is a young variable star in the equatorial constellation of Taurus. It is too faint to be visible to the naked eye with an apparent visual magnitude that ranges from 8.7 to 12.25. The distance to this star is approximately 487 light years based on parallax measurements, and it is drifting further away with a radial velocity of ~23 km/s. It appears to be part of the T-association Tau 4. CQ Tauri lies close enough to the ecliptic to undergo lunar occultations.

References

Sky around the young star MWC 480 The sky around the young star MWC 480.jpg
Sky around the young star MWC 480
  1. ↑ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  2. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 .
  3. 1 2 3 Mendigutía, I.; Mora, A.; Montesinos, B.; Eiroa, C.; Meeus, G.; Merín, B.; Oudmaijer, R. D. (2012). "Accretion-related properties of Herbig Ae/Be stars". Astronomy & Astrophysics. 543: A59. arXiv: 1205.4734 . doi: 10.1051/0004-6361/201219110 . S2CID   59384870.
  4. 1 2 3 4 5 6 Grady, C. A.; Hamaguchi, K.; Schneider, G.; Stecklum, B.; Woodgate, B. E.; McCleary, J. E.; Williger, G. M.; Sitko, M. L.; Ménard, F.; Henning, Th.; Brittain, S.; Troutmann, M.; Donehew, B.; Hines, D.; Wisniewski, J. P.; Lynch, D. K.; Russell, R. W.; Rudy, R. J.; Day, A. N.; Shenoy, A.; Wilner, D.; Silverstone, M.; Bouret, J.-C.; Meusinger, H.; Clampin, M.; Kim, S.; Petre, R.; Sahu, M.; Endres, M.; Collins, K. A. (2010). "Locating the Accretion Footprint on a Herbig Ae Star: MWC 480". The Astrophysical Journal. 719 (2): 1565–1581. Bibcode:2010ApJ...719.1565G. doi: 10.1088/0004-637X/719/2/1565 . hdl: 2060/20110023025 .
  5. 1 2 3 4 5 6 Loomis, Ryan A.; Öberg, Karin I.; Andrews, Sean M.; Bergin, Edwin; Bergner, Jennifer; Blake, Geoffrey A.; Cleeves, L. Ilsedore; Czekala, Ian; Huang, Jane; Le Gal, Romane; Ménard, Francois; Pegues, Jamila; Qi, Chunhua; Walsh, Catherine; Williams, Jonathan P.; Wilner, David J. (2020). "An Unbiased ALMA Spectral Survey of the Lk Ca 15 and MWC 480 Protoplanetary Disks". The Astrophysical Journal. 893 (2): 101. arXiv: 2006.16187 . Bibcode:2020ApJ...893..101L. doi: 10.3847/1538-4357/ab7cc8 . S2CID   219077531.
  6. ↑ Mora, A.; Merín, B.; Solano, E.; Montesinos, B.; De Winter, D.; Eiroa, C.; Ferlet, R.; Grady, C. A.; Davies, J. K.; Miranda, L. F.; Oudmaijer, R. D.; Palacios, J.; Quirrenbach, A.; Harris, A. W.; Rauer, H.; Collier Cameron, A.; Deeg, H. J.; Garzón, F.; Penny, A.; Schneider, J.; Tsapras, Y.; Wesselius, P. R. (2001). "EXPORT: Spectral classification and projected rotational velocities of Vega-type and pre-main sequence stars". Astronomy and Astrophysics. 378: 116. Bibcode:2001A&A...378..116M. doi: 10.1051/0004-6361:20011098 .
  7. ↑ "HD 31648". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 July 2020.
  8. ↑ K. L. Luhman; et al. (2010). "The Disk Population of the Taurus Star-Forming Region". The Astrophysical Journal Supplement Series. 186 (1): 111–174. arXiv: 0911.5457 . Bibcode:2010ApJS..186..111L. doi:10.1088/0067-0049/186/1/111. S2CID   119189843.
  9. ↑ "Catalog of Resolved Circumstellar Disks". Circumstellardisks.org. Archived from the original on 2015-02-05. Retrieved 2015-04-08.
  10. ↑ "Complex Organic Molecules Discovered in Infant Star System". Eso.org. Retrieved 2015-04-08.
  11. ↑ "Complex Organic Molecules Discovered Around Star MWC 480". Science 2.0. 7 April 2015. Retrieved 2015-04-08.
  12. ↑ Teague, Richard; Bae, Jaehan; Aikawa, Yuri; Andrews, Sean M.; Bergin, Edwin A.; Bergner, Jennifer B.; Boehler, Yann; Booth, Alice S.; Bosman, Arthur D.; Cataldi, Gianni; Czekala, Ian; Guzmán, Viviana V.; Huang, Jane; Ilee, John D.; Law, Charles J.; Le Gal, Romane; Long, Feng; Loomis, Ryan A.; Ménard, François; Öberg, Karin I.; Pérez, Laura M.; Schwarz, Kamber R.; Sierra, Anibal; Walsh, Catherine; Wilner, David J.; Yamato, Yoshihide; Zhang, Ke (2021), "Molecules with ALMA at Planet-forming Scales (MAPS). XVIII. Kinematic Substructures in the Disks of HD 163296 and MWC 480", The Astrophysical Journal Supplement Series, 257 (1): 18, arXiv: 2109.06218 , Bibcode:2021ApJS..257...18T, doi: 10.3847/1538-4365/ac1438 , S2CID   237504930
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.