Mikko Tuomi

Last updated
Mikko Tuomi
Born
Espoo, Finland [1]
Citizenship Finland
Alma mater University of Turku
Known for
Scientific career
Institutions University of Turku
University of Hertfordshire
Thesis Multidata inverse problems and Bayesian solution methods in astronomy  (2013)
Doctoral advisor Harry Lehto
Esko Valtaoja

Mikko Tuomi is a Finnish astronomer from the University of Hertfordshire, most known for his contributions to the discovery of a number of exoplanets, among them the Proxima Centauri b which orbits the closest star to the Sun. Mikko Tuomi was the first to find indications of the existence of Proxima Centauri b in archival observation data. [2] Other exoplanets to whose discovery or study Tuomi has contributed include HD 40307, [3] HD 154857 c, [4] Kapteyn c, [5] Gliese 682 c, [6] HD 154857, [4] Gliese 221, [7] Gliese 581 g [8] and the planetary system orbiting Tau Ceti. [9] He has led the development of new data analysis techniques for distinguishing observations caused by natural activity of the star and those caused by planets orbiting them. [10]

Contents

Publications

Mikko Tuomi has contributed to many cosmologist research articles including:

Discoveries

Mikko Tuomi helped discover the Proxima Centauri b planet by observing the gravitational tug of Proxima Centauri's star, Proxima Centauri. [2]

See also

Related Research Articles

<span class="mw-page-title-main">Proxima Centauri</span> Star in the constellation Centaurus

Proxima Centauri is a small, low-mass star located 4.2465 light-years (1.3020 pc) away from the Sun in the southern constellation of Centaurus. Its Latin name means the 'nearest [star] of Centaurus'. It was discovered in 1915 by Robert Innes and is the nearest-known star to the Sun. With a quiescent apparent magnitude of 11.13, it is too faint to be seen with the unaided eye. Proxima Centauri is a member of the Alpha Centauri star system, being identified as component Alpha Centauri C, and is 2.18° to the southwest of the Alpha Centauri AB pair. It is currently 12,950 AU (0.2 ly) from AB, which it orbits with a period of about 550,000 years.

<span class="mw-page-title-main">Gliese 667</span> Triple star system in the constellation Scorpius

Gliese 667 is a triple-star system in the constellation Scorpius lying at a distance of about 7.2 parsecs from Earth. All three of the stars have masses smaller than the Sun. There is a 12th-magnitude star close to the other three, but it is not gravitationally bound to the system. To the naked eye, the system appears to be a single faint star of magnitude 5.89.

<span class="mw-page-title-main">Gliese 581d</span> Contested super-Earth orbiting Gliese 581

Gliese 581d was a candidate extrasolar planet orbiting within the Gliese 581 system, approximately 20.4 light-years away in the Libra constellation. It was the third planet claimed in the system and the fourth or fifth in order from the star. Multiple subsequent studies found that the planetary signal in fact originates from stellar activity, and thus the planet does not exist.

Gliese 832 b is a gas giant exoplanet about 80% the mass of Jupiter, located 16.2 light-years from the Sun in the constellation of Grus, orbiting the red dwarf star Gliese 832.

Gliese 676 is a 10th-magnitude wide binary system of red dwarfs that has an estimated minimum separation of 800 AU with an orbital period of greater than 20,000 years. It is located approximately 54 light years away in the constellation Ara. In 2009, a gas giant was found in orbit around the primary star, in addition to its confirmation in 2011 there was also a strong indication of a companion; the second gas giant was characterised in 2012, along with two much smaller planets.

Gliese 163 is a faint red dwarf star with multiple exoplanetary companions in the southern constellation of Dorado. Other stellar catalog names for it include HIP 19394 and LHS 188. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 11.79 and an absolute magnitude of 10.91. This system is located at a distance of 49.4 light-years from the Sun based on parallax measurements. Judging by its space velocity components, it is most likely a thick disk star.

<span class="mw-page-title-main">HD 40307 g</span> Exoplanet candidate in the constellation of Pictor

HD 40307 g is an exoplanet candidate suspected to be orbiting in the habitable zone of HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany.

<span class="mw-page-title-main">HD 40307 e</span> Extrasolar planet in the constellation Pictor

HD 40307 e is an extrasolar planet candidate suspected to be orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany.

HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany. The existence of planet was confirmed in 2015.

<span class="mw-page-title-main">Tau Ceti e</span> Super-Earth exoplanet orbiting Tau Ceti

Tau Ceti e, also called 52 Ceti e, is an exoplanet orbiting Tau Ceti that was detected by statistical analyses of the data of the star's variations in radial velocity that were obtained using HIRES, AAPS and HARPS. Its possible properties were refined in 2017: it orbits at a distance of 0.552 AU with an orbital period of 168 days and has a minimum mass of 3.93 Earth masses. If Tau Ceti e possesses an Earth-like atmosphere, the surface temperature would be around 68 °C. Based upon the incident flux upon the planet, a study by Güdel et al. (2014) speculated that the planet may lie inside the inner-boundary of the habitable zone and closer to a Venus-like world.

Innes' star is an M3.5-type red dwarf, located in constellation Carina. It has around 35% of the mass of the Sun, yet only 1.1% of its luminosity, and an estimated surface temperature of 3,323 K.

Gliese 422 b is an exoplanet orbiting the red dwarf Gliese 422. Gliese 422 b was discovered in 2014, and discovery was confirmed in 2020. It has a minimum mass of about ten times that of Earth.

<span class="mw-page-title-main">Proxima Centauri b</span> Terrestrial planet orbiting Proxima Centauri

Proxima Centauri b, sometimes referred to as Alpha Centauri Cb, is an exoplanet orbiting within the habitable zone of the red dwarf star Proxima Centauri, which is the closest star to the Sun and part of the larger triple star system Alpha Centauri. It is about 4.2 ly (1.3 pc) from Earth in the constellation Centaurus, making it, along with the currently-disputed Proxima c, and Proxima d the closest known exoplanets to the Solar System.

<span class="mw-page-title-main">Guillem Anglada-Escudé</span> Spanish astronomer

Guillem Anglada-Escudé, is a Catalan astronomer. In 2016, he led a team of astronomers under the Pale Red Dot campaign, which resulted in the confirmation of the existence of Proxima Centauri b, the closest potentially habitable extrasolar planet to Earth, followed by the publication of a peer-reviewed article in Nature. In 2017, Anglada-Escudé was named amongst the 100 most influential people according to Time, and one of Nature's top 10 scientists of the year 2016. He is currently a research fellow at Institut de Ciències de l'Espai.

CD-44 170, also known as Gliese 27.1, Gliese 9018 and HIP 3143, is an M-type main-sequence star. Its surface temperature is 3,604 K ±72 K. The star's concentration of heavy elements is similar to that of the Sun.

References

  1. ↑ Milla Ollikainen (February 10, 2017). "Elämää avaruudessa? Mikko Tuomi löysi planeetan" (in Finnish). Retrieved February 21, 2020.
  2. 1 2 Astronomer, Dr Sten Odenwald; Consortium, NASA Heliophysics Education (2016-08-26). "Proxima Centauri b: Earth-sized? Earth-like? Or Habitable?". The Huffington Post. Retrieved 2016-08-28.
  3. ↑ Tuomi, Mikko; Anglada-Escudé, Guillem; Gerlach, Enrico; Jones, Hugh R. A.; Reiners, Ansgar; Rivera, Eugenio J.; Vogt, Steven S.; Butler, R. Paul (17 December 2012). "Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307". Astronomy & Astrophysics. 549: A48. arXiv: 1211.1617 . Bibcode:2013A&A...549A..48T. doi:10.1051/0004-6361/201220268.
  4. 1 2 The Anglo-Australian Planet Search. XXIII. Two New Jupiter Analogs: Robert A. Wittenmyer, Jonathan Horner, C.G. Tinney, R.P. Butler, H.R.A. Jones, Mikko Tuomi, G.S. Salter, B.D. Carter, F. Elliott Koch, S.J. O'Toole, J. Bailey, D. Wright
  5. ↑ Guillem Anglada-Escudé, Pamela Arriagada, Mikko Tuomi, Mathias Zechmeister, James S. Jenkins, Aviv Ofir, Stefan Dreizler, Enrico Gerlach, Chris J. Marvin, Ansgar Reiners, Sandra V. Jeffers, R. Paul Butler, Steven S. Vogt, Pedro J. Amado, Cristina Rodríguez-López, Zaira M. Berdiñas, Julian Morin, Jeff D. Crane, Stephen A. Shectman, Ian B. Thompson, Matías Díaz, Eugenio Rivera, Luis F. Sarmiento, Hugh R.A. Jones, Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf. (Cornell University 3 June 2014).
  6. ↑ Mikko Tuomi, Hugh R. A. Jones, John R. Barnes, Guillem Anglada-Escudé, James S. Jenkins, Bayesian search for low-mass planets around nearby M dwarfs. Estimates for occurrence rate based on global detectability statistics (Submitted on 3 Mar 2014).
  7. ↑ A new cold sub-Saturnian candidate planet orbiting GJ 221: Mikko Tuomi, January 16, 2014
  8. ↑ Mikko Tuomi (2011). "Bayesian re-analysis of the radial velocities of Gliese 581. Evidence in favour of only four planetary companions". Astronomy & Astrophysics. 528: L5. arXiv: 1102.3314 . Bibcode:2011A&A...528L...5T. doi:10.1051/0004-6361/201015995.
  9. ↑ Tuomi, M.; et al. (March 2013). "Signals embedded in the radial velocity noise: Periodic variations in the Tau Ceti velocities". Astronomy & Astrophysics. 551 (preprint): A79. arXiv: 1212.4277 . Bibcode:2012yCat..35510079T. doi:10.1051/0004-6361/201220509.
  10. ↑ Stephens, Tim: Four Earth-sized planets detected orbiting the nearest sun-like star. Phys.org, August 9, 2017.
  11. ↑ Wittenmyer, Robert A.; Tuomi, Mikko; Butler, R. P.; Jones, H. R. A.; Anglada-Escude, Guillem; Horner, Jonathan; Tinney, C. G.; Marshall, J. P.; Carter, B. D. (2014-06-21). "GJ 832c: A Super-Earth in the Habitable Zone". The Astrophysical Journal. 791 (2): 114. arXiv: 1406.5587 . Bibcode:2014ApJ...791..114W. doi:10.1088/0004-637X/791/2/114. ISSN   0004-637X.
  12. ↑ Anglada-Escude, G.; Arriagada, P.; Tuomi, M.; Zechmeister, M.; Jenkins, J. S.; Ofir, A.; Dreizler, S.; Gerlach, E.; Marvin, C. J. (2014-06-03). "Two planets around Kapteyn's star: a cold and a temperate super-Earth orbiting the nearest halo red dwarf". Monthly Notices of the Royal Astronomical Society: Letters. 443 (1): L89–L93. arXiv: 1406.0818 . Bibcode:2014MNRAS.443L..89A. doi:10.1093/mnrasl/slu076. ISSN   1745-3925.
  13. ↑ Tuomi, M.; Jones, H. R. A.; Barnes, J. R.; Anglada-Escude, G.; Jenkins, J. S. (2014-03-03). "Bayesian search for low-mass planets around nearby M dwarfs - estimates for occurrence rate based on global detectability statistics". Monthly Notices of the Royal Astronomical Society. 441 (2): 1545–1569. arXiv: 1403.0430 . Bibcode:2014MNRAS.441.1545T. doi:10.1093/mnras/stu358. ISSN   0035-8711.
  14. ↑ Anglada-Escudé, Guillem; Tuomi, Mikko; Gerlach, Enrico; Barnes, Rory; Heller, René; Jenkins, James S.; Wende, Sebastian; Vogt, Steven S.; Butler, R. Paul (2013-06-25). "A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone". Astronomy & Astrophysics. 556: A126. arXiv: 1306.6074 . Bibcode:2013A&A...556A.126A. doi:10.1051/0004-6361/201321331. ISSN   0004-6361.
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