HD 100546 – Wikipedia

Posted on by
before-content-x4

From Wikipedia, the free encyclopedia

 after-content-x4

Star in the constellation Musca

HD 100546, is a star 316.4 light-years from Earth.[4] It is orbited by an approximately 20 MJ exoplanet at 6.5 AU,[6] although further examination of the disk profile indicates it might be a more massive object such as a brown dwarf or more than one planet.[7] 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.[8]

Estimated to be around 10 million years old, it is at the upper age limit of the class of stars it belongs to—Herbig Ae/Be stars, and also the nearest example to the Solar System.[5]

Planetary system[edit]

Possible birth of new planet[edit]

 after-content-x4
Artist’s impression of HD 100546 b

In 2013, researchers reported that they had found what seems to be a planet in the process of being formed, embedded in the star’s large disc of gas and dust. If confirmed, it would represent the first opportunity to study the early stages of planet formation observationally.[14]

Evidence for a planetary companion to HD 100546 b was gathered using the UVES echelle spectrograph at the VLT in Chile.[6] This confirms other data indicating a planetary companion. HD 100546 b might be the largest exoplanet discovered with a size of the planet and surrounding disk[8] of around 6.9 RJ; the planet’s mass puts it near the border between a large planet and a brown dwarf.[11][6] This study found an effective temperature of 932+193
−202 K for the observed source.[11]

However, the position where HD 100546 b was detected was inside compared with the gap between the inner and outer disks, and outside compared with the central cavity, so the validity of the planet was shown from the characteristics of the star disk. There was a discrepancy with the discussion. As a result of further detailed observation of the position where HD 100546 b was detected, the light source identified as HD 100546 b appeared to be a point light source in the analysis under specific conditions, but in many cases it became a more diffuse structure. Visible part may be not the planet itself, but the disturbance in disk caused by the much smaller (~10MEarth) planet completely embedded in the dust shroud.[9] The presence of disturbance, possibly created by a forming planet, is also confirmed by the detection of sulphur monoxide, indicating a shockwaves propagating through the gas disk.[15]

Circumstellar disk[edit]

Coronagraphic optical observations with the Hubble Space Telescope[1][5] show complex spiral patterns in the circumstellar disk. The causes of these structures remain uncertain, although spirals are consistent with the instabilities caused by forming planets.[10] The disk colors are similar to those derived for Kuiper Belt objects, suggesting that the same weathering processes are at work in HD 100546. The disk is fairly flat, consistent with an advanced evolutionary state,[1] and have a wide gap at 40–150 AU radii, possibly carved by the outer planet in the gap.[10]

Spectroscopic analysis of mid-IR data taken from OSCIR on the 4 m Blanco Telescope at Cerro Tololo Inter-American Observatory indicates the presence of a small particles (10–18 μm) containing silicates.[5] The material is found at distances out to 17 AU away from the star and has a temperature of approximately 227 K.[5]

See also[edit]

References[edit]

  1. ^ a b c Ardila, D. R.; Golimowski, D. A.; Krist, J. E.; Clmapin, M.; Ford, H. C.; Illingworth, G. D. (2007). “Hubble Space Telescope Advanced Camera for Surveys Coronagraphic Observations of the Dust Surrounding HD 100546”. Astrophysical Journal. 665 (1): 512–534. arXiv:0704.1507. Bibcode:2007ApJ…665..512A. doi:10.1086/519296. S2CID 41469182.
  2. ^ “The Birth of a Giant Planet?”. ESO. Retrieved 3 April 2013.
  3. ^ a b c d “HD 100546”. SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 March 2018.
  4. ^ a b c d e f van Leeuwen, F. (2007). “Validation of the new Hipparcos reduction”. Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A…474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.Vizier catalog entry
  5. ^ a b c d e Grady, C. A.; et al. (2001). “The Disk and Environment of the Herbig Be Star HD 100546”. The Astronomical Journal. 122 (6): 3396–3406. Bibcode:2001AJ….122.3396G. doi:10.1086/324447.
  6. ^ a b c Acke, B.; van der Ancker, M. (November 2005). “Resolving the disk rotation of HD 97048 and HD 100546 in the [O I] 6300A line: evidence for a giant planet orbiting HD 100546”. Astronomy and Astrophysics. 449 (267): 267. arXiv:astro-ph/0512562. Bibcode:2006A&A…449..267A. doi:10.1051/0004-6361:20054330. S2CID 10148216.
  7. ^ Mulders, Gijs D.; Paardekooper, Sijme-Jan; Pani´c, Olja; Dominik, Carsten; et al. (2013). “Planet or Brown Dwarf? Inferring the Companion Mass in HD 100546 from the Wall Shape using Mid-Infrared Interferometry”. Astronomy & Astrophysics. 557A (A68): 10. arXiv:1306.4264. Bibcode:2013A&A…557A..68M. doi:10.1051/0004-6361/201220930. S2CID 9014058.
  8. ^ a b c Quanz, Sasch P.; Amara, Adam; Meyer, Michael P.; Kenworthy, Matthew P.; et al. (2013). “A young protoplanet candidate embedded in the circumstellar disk of HD 100546”. Astrophysical Journal. 766 (1). L1. arXiv:1302.7122. Bibcode:2013ApJ…766L…1Q. doi:10.1088/2041-8205/766/1/l1. S2CID 56140977.
  9. ^ a b Casassus, Simon; Cárcamo, Miguel; Hales, Antonio; Weber, Philipp; Dent, Bill (2022), “The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches”, The Astrophysical Journal Letters, 933: L4, arXiv:2206.03236, doi:10.3847/2041-8213/ac75e8, S2CID 249431595
  10. ^ a b c d e f Fedele, D.; Toci, C.; Maud, L.; Lodato, G. (2021), “ALMA 870 μm continuum observations of HD 100546”, Astronomy & Astrophysics, 651: A90, arXiv:2106.07757, doi:10.1051/0004-6361/202141278, S2CID 243181865
  11. ^ a b c Quanz, Sasch P.; Amara, Adam; Meyer, Michael P.; Kenworthy, Matthew P.; et al. (2014). “Confirmation and characterization of the protoplanet HD100546 b – Direct evidence for gas giant planet formation at 50 au”. Astrophysical Journal. 807 (1). 64. arXiv:1412.5173. Bibcode:2015ApJ…807…64Q. doi:10.1088/0004-637X/807/1/64. S2CID 119119314.
  12. ^ Quanz, Sascha P.; Amara, Adam; Meyer, Michael R.; Girard, Julien H.; Kenworthy, Matthew A.; Kasper, Markus (2015-07-01). “Confirmation and Characterization of the Protoplanet HD 100546 b—Direct Evidence for Gas Giant Planet Formation at 50 AU”. The Astrophysical Journal. 807: 64. Bibcode:2015ApJ…807…64Q. doi:10.1088/0004-637X/807/1/64. ISSN 0004-637X. S2CID 119119314.
  13. ^ Rameau, Julien; Follette, Katherine B.; Pueyo, Laurent; Marois, Christian; Macintosh, Bruce; Millar-Blanchaer, Maxwell; Wang, Jason J.; Vega, David; Doyon, René; Lafrenière, David; Nielsen, Eric L.; Bailey, Vanessa; Chilcote, Jeffrey K.; Close, Laird M.; Esposito, Thomas M. (2017-06-01). “An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO”. The Astronomical Journal. 153 (6): 244. Bibcode:2017AJ….153..244R. doi:10.3847/1538-3881/aa6cae. hdl:10150/624214. ISSN 0004-6256. S2CID 19100982.
  14. ^ “Is HD 100546 showing us the birth of a giant planet?”. Science Codex. 2013-02-28. Archived from the original on 2013-03-05. Retrieved 2013-03-01.
  15. ^ Booth, Alice S.; Ilee, John D.; Walsh, Catherine; Kama, Mihkel; Keyte, Luke; Van Dishoeck, Ewine F.; Nomura, Hideko (2023), “Sulphur monoxide emission tracing an embedded planet in the HD 100546 protoplanetary disk”, Astronomy & Astrophysics, 669: A53, arXiv:2210.14820, doi:10.1051/0004-6361/202244472, S2CID 253116975
  1. ^ The size of planet cannot be determined in size as flux from planet and disk are superimposed.

Further reading[edit]

External links[edit]



after-content-x4