Astronomy:HD 100546

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Short description: Star in the constellation Musca
HD 100546
View of the dust disc around the young star HD 100546.jpg
This image from the NASA/ESA Hubble Space Telescope shows a visible light view of the outer dust around the young star HD 100546, with the newly discovered protoplanet positioned and marked by an orange spot. Artifacts from the brilliant central star dominate the inner part of this picture, which has been digitally subtracted. Black blobs are also artifacts.[1][2]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Musca
Right ascension  11h 33m 25.441s[4]
Declination −70° 11′ 41.24″[4]
Apparent magnitude (V) 6.68 – 6.87[5]
Characteristics
Evolutionary stage Herbig Ae/Be star[6]
Spectral type kB8 – A0Vae[7][3]
Apparent magnitude (B) 6.71±0.01[8]
Apparent magnitude (V) 6.30[9]
Apparent magnitude (G) 6.686±0.003[4]
Apparent magnitude (I) 6.64±0.05[1]
Apparent magnitude (J) 6.425±0.020[10]
Apparent magnitude (H) 5.96±0.03[10]
Apparent magnitude (K) 5.418±0.023[10]
Astrometry
Radial velocity (Rv)9.10±1.2[11] km/s
Proper motion (μ) RA: −38.730(46)[4] mas/yr
Dec.: −0.097(39)[4] mas/yr
Parallax (π)9.2494 ± 0.0375[4] mas
Distance353 ± 1 ly
(108.1 ± 0.4 pc)
Details
Mass2.18+0.02
−0.17[12] M☉
Radius1.5±0.1[13] R☉
Luminosity19.5+7.42
−5.37[lower-alpha 1][13] L☉
Surface gravity (log g)–4.0[14] cgs
Temperature9,800[14] K
Metallicity [Fe/H]–1.0[7] – –1.4±0.2[15] dex
Age4.8+2.0
−1.1[14] Myr
Other designations
KR Mus, HIP 56379,[3] SAO 251457, CD−69° 893
Database references
SIMBADdata

HD 100546, also known as KR Muscae, is a pre-main sequence star of spectral type B8 to A0 located 353 light-years (108 parsecs) from Earth in the southern constellation of Musca.[4] 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.[16]

Estimated to be less than 10 million years old, it belongs to Herbig Ae/Be stars, and also the nearest example to the Solar System.[14][17]

Planetary system

The HD 100546 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
Inner disk 0.2–4 AU 33±11[18]° —
d[19] (disputed) 33–71[20] MJ 7.8[19] — — — —
c (disputed) 15[18] MJ 10[6] — — — 1.265[18] RJ
Outer disk 13[21]–400[22] AU 44±8[18]° —
candidate 1 (unconfirmed) 8[23] MJ 13[23] — — — —
b[16] (disputed[24]) 1.65[14] MJ 53±2[21] — — — 3.4[25] RJ
candidate 2 (unconfirmed) 3[23] MJ 143[23] — — — —

The HD 100546 system as a whole has one confirmed protoplanet candidate and there is evidence for 1–2 others, thus it is considered an important evolutionary precursor to intermediate-mass stars with multiple super-jovian planets at moderate/wide separations like HR 8799.[26] While other hypothetical planets have been claimed to exist around the star, none of the discoveries have been confirmed.

Planet b

Artist's impression of the protoplanet HD 100546 b[27] forming in its parent star's protoplanetary disc.

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.[28] The flux from HD 100546 b[16] and its circumplanetary disk (CPD) are superimposed, leaving its properties such the radius and temperature thus very uncertain.[21]

Various estimates for the mass of HD 100546 b has been varying between 1 and 25 MJ.[29][25] Although standard hot-start models imply a mass of approximately 15 Jupiter mass, other models and HD 100546 b's H-band photometry implies masses below 10 Jupiter mass for a 1-million-years-old newly born planet or if made visible by its CPD, while older ages suggest higher masses.[26][21]

More recently, a 2019 study placed an upper limit for the planetary mass was given to be as low as 1.65 Jupiter mass based on the relation between the planet, CPD, and circumstellar disk (CSD) masses derived from numerical simulation.[14] The CPD has been assumed to be optically thin with derived upper mass and radius limits of 1.44 times as massive as Earth (M⊕) and 0.44 astronomical unit (AU), while the mass of CSD was given to be 50 Jupiter mass.[14] While gas-starved models are also still compatible, this would suggest that HD 100546 b is inconsistent with several planet accretion models.[14]

Fitting a single temperature blackbody to the observed fluxes of the point source component gives a very large radius of 6.9+2.7
−2.9 times that of Jupiter (|♃|J}}}}}}) and an effective temperature of 932+193
−202 K for the emitting area surrounding the embedded protoplanet respectively.[21] This large radius refers to the diffuse dust and gas envelope or debris disk surrounding the planet, not the planet itself; these estimates are mistakenly used as a single planetary radius and effective temperature for HD 100546 b by the NASA Exoplanet Archive. A best-fit luminosity was also found by the same study to be 2.3+0.6
−0.4×10−4 times as luminous as the Sun (L☉).[21]

Despite the uncertainty of the planet's properties, a 2017 study calculated HD 100546 b as a very highly reddened substellar object with a good-fit effective temperature of 2,630 K and a planetary mass and radius of 25 MJup and 3.4 RJup, making it still nonetheless one of the largest exoplanets discovered by size.[25] However, it has been predicted by planetary evolutionary theory that gas giants including hot Jupiters typically cannot exceed 2.2 RJ and that more massive gas giants would have lower radius at the time of their formation. This mass would put the planet beyond the border between a large planet and a brown dwarf.

Planet c

In April of 2003, another planetary companion candidate was proposed and evidence was later gathered using the UVES echelle spectrograph at the VLT in Chile in 2005.[30] This confirms other data indicating a planetary companion with a mass approximately 20 |♃|J}}}}}} and a distance of 6.5 AU from HD 100546,[30] 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.[6]

The same planetary companion, dubbed "HD 100546 c",[19][29] was observed in 2014, and is calculated to have a mass estimated to be between 5 MJ and 20 MJ.[31][29] With an estimated distance roughly 13 AU from HD 100546, circumstantial evidence suggests that HD 100546 c may be responsible for clearing out the inner disk cavity, although it would have been rapidly accreting gas, and thus it would be unusually bright.[29] It was also expected to be surrounded by a circumplanetary disk of about 0.1 AU in radius.[31] The planet is calculated to have an accretion rate up to 10−8 M☉ per year assuming a planetary mass of 15 MJup, which would correspond to a planetary radius of 0.13 R☉ based on evolutionary tracks.[18] Thus, HD 100546 c is either in a relatively quiescent stage or its growth from accretion is at a low level or has already ceased.[18] The presence of disturbance, possibly created by HD 100546 c, is also confirmed by the detection of sulphur monoxide, indicating a shockwaves propagating through the gas disk.[32]

The position where HD 100546 c 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. This companion candidate has been contested, however, and it may be a weakly polarized disk feature instead.

Planet d

ALMA observations at 1.3 mm have revealed a point source at a position angle of 37° and a projected separation of 7.8 AU, which could represent an additional planetary candidate, hereafter HD 100546 d.[19]

Hypothetical planets

A disturbance in disk may have been caused by a ~10 M⊕ planet completely embedded in the dust shroud.[12]

Circumstellar disk

Coronagraphic optical observations with the Hubble Space Telescope[1][17] 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.[27] 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 an outer planet in the gap.[27]

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.[17] The material is found at distances out to 17 AU away from the star and has a temperature of approximately 227 K.[17]

See also

Notes

  1. ↑ The luminosity of HD 100546 is log(L/L☉) = 1.29+0.14
    −0.14    .

References

  1. ↑ 1.0 1.1 1.2 1.3 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. doi:10.1086/519296. Bibcode: 2007ApJ...665..512A. 
  2. ↑ "The Birth of a Giant Planet?". ESO. http://www.eso.org/public/news/eso1310/. 
  3. ↑ 3.0 3.1 3.2 "HD 100546". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+100546. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  5. ↑ "GCVS Query=KR Mus". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. http://www.sai.msu.su/gcvs/cgi-bin/search.cgi?search=KR+Mus. 
  6. ↑ 6.0 6.1 6.2 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. doi:10.1051/0004-6361/201220930. Bibcode: 2013A&A...557A..68M. 
  7. ↑ 7.0 7.1 Gray, R. O.; Riggs, Q. S.; Koen, C.; Murphy, S. J.; Newsome, I. M.; Corbally, C. J.; Cheng, K. -P.; Neff, J. E. (2017). "The Discovery of λ Bootis Stars: The Southern Survey I". The Astronomical Journal 154 (1): 31. doi:10.3847/1538-3881/aa6d5e. Bibcode: 2017AJ....154...31G. https://pure.au.dk/ws/files/134370733/The_Discovery_of_Bootis_Stars_The_Southern_Survey_I.pdf. 
  8. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355. Bibcode: 2000A&A...355L..27H. 
  9. ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". Vizier Online Data Catalog. Bibcode: 2002yCat.2237....0D. 
  10. ↑ 10.0 10.1 10.2 Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". Vizier Online Data Catalog. Bibcode: 2003yCat.2246....0C. 
  11. ↑ Kharchenko, N. V.; Scholz, R. -D.; Piskunov, A. E.; Röser, S.; Schilbach, E. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ∼55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten 328 (9): 889. doi:10.1002/asna.200710776. Bibcode: 2007AN....328..889K. 
  12. ↑ 12.0 12.1 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 (1): L4, doi:10.3847/2041-8213/ac75e8, Bibcode: 2022ApJ...933L...4C 
  13. ↑ 13.0 13.1 Fairlamb, J. R.; Oudmaijer, R. D.; Mendigutía, I.; Ilee, J. D.; Van Den Ancker, M. E. (2015). "A spectroscopic survey of Herbig Ae/Be stars with X-shooter – I. Stellar parameters and accretion rates". Monthly Notices of the Royal Astronomical Society 453: 976–1001. doi:10.1093/mnras/stv1576. 
  14. ↑ 14.0 14.1 14.2 14.3 14.4 14.5 14.6 14.7 Pineda, Jaime E.; Szulágyi, Judit; Quanz, Sascha P.; Van Dishoeck, Ewine F.; Garufi, Antonio; Meru, Farzana; Mulders, Gijs D.; Testi, Leonardo et al. (2019). "High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits". The Astrophysical Journal 871 (1): 48. doi:10.3847/1538-4357/aaf389. Bibcode: 2019ApJ...871...48P. 
  15. ↑ Guimarães, M. M.; Alencar, S. H. P.; Corradi, W. J. B.; Vieira, S. L. A. (2006). "Stellar parameters and evidence of circumstellar activity for a sample of Herbig Ae/Be stars". Astronomy & Astrophysics 457 (2): 581–589. doi:10.1051/0004-6361:20065005. Bibcode: 2006A&A...457..581G. 
  16. ↑ 16.0 16.1 16.2 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. doi:10.1088/2041-8205/766/1/l1. Bibcode: 2013ApJ...766L...1Q. 
  17. ↑ 17.0 17.1 17.2 17.3 Grady, C. A. et al. (2001). "The Disk and Environment of the Herbig Be Star HD 100546". The Astronomical Journal 122 (6): 3396–3406. doi:10.1086/324447. Bibcode: 2001AJ....122.3396G. 
  18. ↑ 18.0 18.1 18.2 18.3 18.4 18.5 Mendigutía, I.; Oudmaijer, R. D.; Garufi, A.; Lumsden, S. L.; Huélamo, N.; Cheetham, A.; De Wit, W. J.; Norris, B. et al. (2017). "The protoplanetary system HD 100546 in H α polarized light from SPHERE/ZIMPOL". Astronomy & Astrophysics 608: A104. doi:10.1051/0004-6361/201731131. 
  19. ↑ 19.0 19.1 19.2 19.3 Petit Dit de la Roche, D. J. M.; Oberg, N.; Van Den Ancker, M. E.; Kamp, I.; Van Boekel, R.; Fedele, D.; Ivanov, V. D.; Kasper, M. et al. (2021). "New mid-infrared imaging constraints on companions and protoplanetary disks around six young stars". Astronomy & Astrophysics 648: A92. doi:10.1051/0004-6361/202039261. Bibcode: 2021A&A...648A..92P. 
  20. ↑ Pérez, Sebastián; Casassus, Simon; Hales, Antonio; Marino, Sebastián; Cheetham, Anthony; Zurlo, Alice; Cieza, Lucas; Dong, Ruobing et al. (2020). "Long Baseline Observations of the HD 100546 Protoplanetary Disk with ALMA". The Astrophysical Journal 889 (1): L24. doi:10.3847/2041-8213/ab6b2b. Bibcode: 2020ApJ...889L..24P. 
  21. ↑ 21.0 21.1 21.2 21.3 21.4 21.5 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. doi:10.1088/0004-637X/807/1/64. Bibcode: 2015ApJ...807...64Q. 
  22. ↑ Pinilla, P.; Birnstiel, T.; Walsh, C. (2015). "Sequential planet formation in the HD 100546 protoplanetary disk?". Astronomy & Astrophysics 580: A105. doi:10.1051/0004-6361/201425539. Bibcode: 2015A&A...580A.105P. 
  23. ↑ 23.0 23.1 23.2 23.3 Pyerin, Max Ackermann; Delage, Timmy N.; Kurtovic, Nicolás T.; Gárate, Matías; Henning, Thomas; Pinilla, Paola (2021). "Constraining the properties of the potential embedded planets in the disk around HD 100546". Astronomy & Astrophysics 656: A150. doi:10.1051/0004-6361/202141998. Bibcode: 2021A&A...656A.150P. 
  24. ↑ Rameau, Julien; Follette, Katherine B.; Pueyo, Laurent; Marois, Christian; Macintosh, Bruce; Millar-Blanchaer, Maxwell; Wang, Jason J.; Vega, David et al. (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. doi:10.3847/1538-3881/aa6cae. ISSN 0004-6256. Bibcode: 2017AJ....153..244R. 
  25. ↑ 25.0 25.1 25.2 Sissa, Elena (2017). Observation of extrasolar planets at various ages. Bibcode: 2017PhDT.......406S. 
  26. ↑ 26.0 26.1 Currie, Thayne; Muto, Takayuki; Kudo, Tomoyuki; Honda, Mitsuhiko; Brandt, Timothy D.; Grady, Carol; Fukagawa, Misato; Burrows, Adam et al. (2014). "RECOVERY OF THE CANDIDATE PROTOPLANET HD 100546 b WITH GEMINI/NICI AND DETECTION OF ADDITIONAL (PLANET-INDUCED?) DISK STRUCTURE AT SMALL SEPARATIONS". The Astrophysical Journal 796 (2): L30. doi:10.1088/2041-8205/796/2/L30. Bibcode: 2014ApJ...796L..30C. 
  27. ↑ 27.0 27.1 27.2 Fedele, D.; Toci, C.; Maud, L.; Lodato, G. (2021), "ALMA 870 μm continuum observations of HD 100546", Astronomy & Astrophysics 651: A90, doi:10.1051/0004-6361/202141278 
  28. ↑ "Is HD 100546 showing us the birth of a giant planet?". Science Codex. 2013-02-28. http://www.sciencecodex.com/the_birth_of_a_giant_planet-107687. 
  29. ↑ 29.0 29.1 29.2 29.3 Currie, Thayne; Cloutier, Ryan; Brittain, Sean; Grady, Carol; Burrows, Adam; Muto, Takayuki; Kenyon, Scott J.; Kuchner, Marc J. (2015). "Resolving the Hd 100546 Protoplanetary System with the Gemini Planet Imager: Evidence for Multiple Forming, Accreting Planets". The Astrophysical Journal 814 (2): L27. doi:10.1088/2041-8205/814/2/L27. Bibcode: 2015ApJ...814L..27C. 
  30. ↑ 30.0 30.1 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. doi:10.1051/0004-6361:20054330. Bibcode: 2006A&A...449..267A. 
  31. ↑ 31.0 31.1 Brittain, Sean D.; Carr, John S.; Najita, Joan R.; Quanz, Sascha P.; Meyer, Michael R. (2014). "NIR SPECTROSCOPY OF THE HAeBe STAR HD 100546. III. FURTHER EVIDENCE OF AN ORBITING COMPANION?". The Astrophysical Journal 791 (2): 136. doi:10.1088/0004-637X/791/2/136. Bibcode: 2014ApJ...791..136B. 
  32. ↑ 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, doi:10.1051/0004-6361/202244472, Bibcode: 2023A&A...669A..53B 

Further reading

  • Van Den Ancker, M. E.; The, P. S.; Tjin a Djie, H. R. E.; Catala, C.; De Winter, D.; Blondel, P. F. C.; Waters, L. B. F. M. (1997). "HIPPARCOS data on Herbig Ae/Be stars: An evolutionary scenario". Astronomy and Astrophysics 324. Bibcode: 1997A&A...324L..33V. 
  • Butler, R. P. et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505–522. doi:10.1086/504701. Bibcode: 2006ApJ...646..505B. 
  • Ecuvillon, A.; Israelian, G.; Pont, F.; Santos, N. et al. (August 2006). "Kinematics of planet-host stars and their relation to dynamical streams in the solar neighbourhood". Astronomy and Astrophysics 461 (171): 171–182. doi:10.1051/0004-6361:20065872. Bibcode: 2007A&A...461..171E. 
  • Jones, B.; Sleep, P.; Underwood, D. (June 2006). "Habitability of known exoplanetary systems based on measured stellar properties". The Astrophysical Journal 649 (1010): 1010–1019. doi:10.1086/506557. Bibcode: 2006ApJ...649.1010J. 
  • Mandell, Avi M.; Raymond, Sean N.; Sigurdsson, Steinn (May 2007). "Formation of Earth-like Planets During and After Giant Planet Migration". The Astrophysical Journal 660 (1): 823–844. doi:10.1086/512759. Bibcode: 2007ApJ...660..823M. 
  • Marchi, S. (May 2007). "Extrasolar planet taxonomy: a new statistical approach". The Astrophysical Journal 666 (1): 475–485. doi:10.1086/519760. Bibcode: 2007ApJ...666..475M. 
  • Hedrick, C. H.; Doering, R.; Lee, K.-G.; Sosey, M. et al. (December 2005). "The Circumstellar Dust Disk of HD 100546". Bulletin of the American Astronomical Society 37 (4): 1167. Bibcode: 2005AAS...207.1009H. 

External links

Coordinates: Sky map 11h 33m 25.4408s, −70° 11′ 41.239″



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