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Ross 128

Coordinates:Sky map11h47m44.4s,+00° 48′ 16″
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Ross 128

Artist's impression of the planetRoss 128 b,with the star Ross 128 visible in the background[1]
Credit:European Southern Observatory
Observation data
EpochJ2000EquinoxJ2000
Constellation Virgo
Right ascension 11h47m44.39727s[2]
Declination +00° 48′ 16.4003″[2]
Apparent magnitude(V) 11.13[3]
Characteristics
Evolutionary stage Main sequence
Spectral type M4V[4]
U−Bcolor index +2.685[5]
B−Vcolor index +1.59[6]
Variable type Flare star[7]
Astrometry
Radial velocity(Rv)−31.0[8][9]km/s
Proper motion(μ)RA:607.299±0.034mas/yr[2]
Dec.:−1223.028±0.023mas/yr[2]
Parallax(π)296.3053 ± 0.0302mas[2]
Distance11.007 ± 0.001ly
(3.3749 ± 0.0003pc)
Absolute magnitude(MV)13.53[3]
Details
Mass0.176±0.004[10]M☉
Radius0.198±0.007[10]R☉
Luminosity (bolometric)0.00366 ± 0.00005[10]L☉
Surface gravity(logg)3.40[11]cgs
Temperature3,189+55
−53[10]K
Metallicity[Fe/H]−0.02±0.08[12]dex
Rotational velocity(vsini)2.1±1.0[13]km/s
Age5.0[14]Gyr
Other designations
FI Virginis, FI Vir,G010-050,GCTP2730,GJ447,HIP57548,LHS315,Vyssotsky286, LTT 13240, LFT 852,LSPMPM I11477+0048.[15]
Database references
SIMBADdata
Ross 128 is located in the constellation Virgo.
Ross 128 is located in the constellation Virgo.
Ross 128
Location of Ross 128 in the constellationVirgo

Ross 128is ared dwarfin theequatorialzodiacconstellationofVirgo,nearβ Virginis.Theapparent magnitudeof Ross 128 is 11.13,[3]which is too faint to be seen with the unaided eye. Based uponparallaxmeasurements, the distance of this star from Earth is 11.007light-years(3.375parsecs), making it the twelfthclosest stellar systemto theSolar System.It was first cataloged in 1926 by American astronomerFrank Elmore Ross.[16]

Properties

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Distances of thenearest starsfrom 20,000 years ago until 80,000 years in the future

This low-mass star has astellar classificationof M4 V,[4]which places it among the category of stars known as red dwarfs. It has about 18%[10]of the mass of the Sun and 20%[10]of the Sun's radius, but generates energy so slowly that it has only 0.033% of the Sun's visible luminosity;[3]however, most of the energy being radiated by the star is in theinfrared band,with thebolometric luminositybeing equal to 0.37% of solar.[10]This energy is being radiated from the star'souter atmosphereat aneffective temperatureof 3,180 K.[4]This gives it the cool orange-red glow of anM-type star.

Ross 128 is anold disk star,which means it has a low abundance of elements other than hydrogen and helium, what astronomers term the star'smetallicity,and it orbits near the plane of theMilky Waygalaxy.[17]The star lacks a strong excess of infrared radiation. Aninfrared excessis usually an indicator of adust ringin orbit around the star.[18][19]

Light curvesfor a flare on FI Virginis, seen in ultraviolet, blue andvisual bandlight, adapted from Lee and Hoxie (1972),[20]

In 1972, a flare was detected from Ross 128. It was observed to increase in brightness by about half a magnitude in theultravioletUband, returning to normal brightness in less than an hour. At optical wavelengths, the brightness changes were almost undetectable.[20]It was classified as aflare starand given thevariable star designationFI Virginis.[21]Because of the low rate of flare activity, it is thought to be a magnetically evolved star. That is, there is some evidence that themagnetic brakingof the star's stellar wind has lowered the frequency of flares, but not the net yield.[22]

Brightness variations thought to be due to rotation of the star and magnetic cycles similar to thesunspot cyclehave also been detected. These cause changes of just a few thousandths of a magnitude. The rotation period is found to be 165.1 days, and the magnetic cycle length 4.1 years.[23]

Ross 128 is orbiting through the galaxy with aneccentricityof 0.122, causing its distance from theGalactic Centerto range between 26.8–34.2kly(8.2–10.5kpc).[24]This orbit will bring the star closer to theSolar Systemin the future. The nearest approach will occur in approximately 71,000 years, when it will come within 6.233 ± 0.085 ly (1.911 ± 0.026 pc).[9]

Planetary system

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Main article:Ross 128 b
The Ross 128 planetary system[25][26]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 1.8+0.56
−0.43M🜨 		0.0493±0.0017 9.8596±0.0056 0.036±0.092 — 1.6+1.1
−0.65R🜨

Ross 128 b was discovered in July 2017 by theHARPSinstrument at theLa Silla Observatoryin Chile, by measuring changes inradial velocityof the host star. Its existence was confirmed on 15 November 2017. It is the second-closest known Earth-size exoplanet, afterProxima b.[27]It is calculated that Ross 128 b has a mass of 1.8 times the Earth, a radius 1.6 times that of the Earth, and orbits 20 times closer to its star than Earth orbits the Sun, intercepting only about 1.38 times more solar radiation than Earth,[26][25][28]increasing the chance of retaining an atmosphere over a geological timescale. Ross 128 b is a closely orbiting planet, with a year (orbital period) lasting about 9.9 days.[29][30]At that close distance from its host star, the planet is most likelytidally locked,meaning that one side of the planet would have eternal daylight and the other would be in darkness.[31][32]Near-infrared high-resolution spectra fromAPOGEEhave demonstrated that Ross 128 has near solar metallicity; Ross 128 b therefore most likely contains rock and iron. Furthermore, recent models generated with these data support the conclusion that Ross 128 b is a "temperate exoplanet in the inner edge of the habitable zone."[33]

Radio signals

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In the spring of 2017, Arecibo astronomers detected strange radio signals thought to originate from Ross 128 that were unlike any they had seen before.[34]SETI's Allen Telescope Array was used for follow-up observations and was unable to detect the signal but did detect man made interference, making it seem clear that the Arecibo detections were due to transmissions from Earth satellites in geosynchronous orbit. Ross 128 has a declination (a coordinate which can be likened to latitude) of close to 0 degrees, which places it in the thick of a phalanx of these satellites. Therefore, it can be concluded that the signal was a result of man-made interference.[35]

See also

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References

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  1. ^"Closest Temperate World Orbiting Quiet Star Discovered – ESO's HARPS instrument finds Earth-mass exoplanet around Ross 128".eso.org.Retrieved15 November2017.
  2. ^abcdVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  3. ^abcdThe One Hundred Nearest Star Systems,Research Consortium on Nearby Stars, 2012-01-01,retrieved2017-11-15
  4. ^abcGautier, Thomas N. III; et al. (2004), "Far Infrared Properties of M Dwarfs",Bulletin of the American Astronomical Society,36:1431,Bibcode:2004AAS...205.5503G
  5. ^Rufener, F. (October 1976), "Second catalogue of stars measured in the Geneva Observatory photometric system",Astronomy & Astrophysics Supplement Series,26:275–351,Bibcode:1976A&AS...26..275R
  6. ^Warren, W. H. Jr. (1978), "Photoelectric Photometric Catalogue of Homogeneous Means in the UBV System",Observatory,Geneva
  7. ^Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)".VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S.1.Bibcode:2009yCat....102025S.
  8. ^Gontcharov, G. A. (2006),Pulkovo Compilation of Radial Velocities for 35493 Hipparcos Stars,retrieved2010-04-18
  9. ^abGarcía-Sánchez, J.; et al. (2001), "Stellar encounters with the solar system",Astronomy and Astrophysics,379(2): 634–659,Bibcode:2001A&A...379..634G,doi:10.1051/0004-6361:20011330
  10. ^abcdefgPineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021)."The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars".The Astrophysical Journal.918(1): 23.arXiv:2106.07656.Bibcode:2021ApJ...918...40P.doi:10.3847/1538-4357/ac0aea.S2CID235435757.40.
  11. ^Rodonò, Marcello, "The Atmospheres of M Dwarfs: Observations",The M-Type Stars,Washington: NASA, pp. 409–453
  12. ^Mann, Andrew W.; et al. (May 2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius".The Astrophysical Journal.804(1): 38.arXiv:1501.01635.Bibcode:2015ApJ...804...64M.doi:10.1088/0004-637X/804/1/64.S2CID19269312.Vizier catalogue entry
  13. ^Fouqué, Pascal; et al. (April 2018)."SPIRou Input Catalogue: global properties of 440 M dwarfs observed with ESPaDOnS at CFHT".Monthly Notices of the Royal Astronomical Society.475(2): 1960–1986.arXiv:1712.04490.Bibcode:2018MNRAS.475.1960F.doi:10.1093/mnras/stx3246.
  14. ^McIntyre, S. R. N. (2022). "Tidally driven tectonic activity as a parameter in exoplanet habitability".Astronomy and Astrophysics.662:A15.arXiv:2204.03501.Bibcode:2022A&A...662A..15M.doi:10.1051/0004-6361/202141112.S2CID248005961.
  15. ^Mann, Andrew W.; Feiden, Gregory A.; Gaidos, Eric; Boya gian, Tabetha; Braun, Kaspar von (4 May 2015)."How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius".The Astrophysical Journal.804(1): 64.arXiv:1501.01635.Bibcode:2015ApJ...804...64M.doi:10.1088/0004-637X/804/1/64.hdl:2152/34940.S2CID19269312.
  16. ^Ross, Frank E. (1926), "New proper-motion stars, (second list)",Astronomical Journal,36(856): 124–128,Bibcode:1926AJ.....36..124R,doi:10.1086/104699
  17. ^Sánchez, F. (1990), Vazquez, M. (ed.),New windows to the universe,vol. 2, Cambridge University Press, p. 313,ISBN0-521-38429-X
  18. ^Jura, M.; et al. (September 2004), "Mid-Infrared Spectra of Dust Debris around Main-Sequence Stars",The Astrophysical Journal Supplement Series,154(1): 453–457,arXiv:astro-ph/0405632,Bibcode:2004ApJS..154..453J,doi:10.1086/422975,S2CID396660
  19. ^Gautier, Thomas N. III; et al. (September 2007), "Far-Infrared Properties of M Dwarfs",The Astrophysical Journal,667(1): 527–536,arXiv:0707.0464,Bibcode:2007ApJ...667..527G,doi:10.1086/520667,S2CID15732144
  20. ^abLee, T. A; Hoxie, D. T (1972). "The Observation of a Stellar Flare in the dM5 Star Ross 128".Information Bulletin on Variable Stars.707:1.Bibcode:1972IBVS..707....1L.
  21. ^Kukarkin, B. V; Kholopov, P. N; Kukarkina, N. P; Perova, N. B (1975). "60th Name-List of Variable Stars".Information Bulletin on Variable Stars.961:1.Bibcode:1975IBVS..961....1K.
  22. ^Skumanich, Andrew (1986-10-15), "Some evidence on the evolution of the flare mechanism in dwarf stars",Astrophysical Journal, Part 1,309:858–863,Bibcode:1986ApJ...309..858S,doi:10.1086/164654
  23. ^Stelzer, B; Damasso, M; Scholz, A; Matt, S. P (2016)."A path towards understanding the rotation-activity relation of M dwarfs with K2 mission, X-ray and UV data".Monthly Notices of the Royal Astronomical Society.463(2): 1844.arXiv:1607.03049.Bibcode:2016MNRAS.463.1844S.doi:10.1093/mnras/stw1936.S2CID55906368.
  24. ^Allen, C.;Herrera, M. A. (1998), "The galactic orbits of nearby UV Ceti stars",Revista Mexicana de Astronomía y Astrofísica,34:37–46,Bibcode:1998RMxAA..34...37A
  25. ^abBonfils, Xavier (2017). "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs".Astronomy and Astrophysics.613:A25.arXiv:1711.06177.Bibcode:2018A&A...613A..25B.doi:10.1051/0004-6361/201731973.S2CID37148632.
  26. ^abTasker, Elizabeth J.;Laneuville, Matthieu; Guttenberg, Nicholas (7 January 2020)."Estimating Planetary Mass with Deep Learning".The Astronomical Journal.159(2): 41.arXiv:1911.11035.Bibcode:2020AJ....159...41T.doi:10.3847/1538-3881/ab5b9e.ISSN1538-3881.S2CID208267900.
  27. ^Koren, Marina (15 November 2017)."An Earth-Sized Exoplanet in Our Cosmic Neighborhood".The Atlantic.The Atlantic Monthly Group.Retrieved15 November2017.
  28. ^Nearby planet is 'excellent' target in search for life.Paul Rincon,BBC News.15 November 2017.
  29. ^Bonfils, Xavier (2017). "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs".Astronomy and Astrophysics.613:A25.arXiv:1711.06177.Bibcode:2018A&A...613A..25B.doi:10.1051/0004-6361/201731973.S2CID37148632.
  30. ^A potentially habitable planet has been discovered just 11 light-years away.John Wenz,Astronomy Magazine.15 November 2017.
  31. ^Nearby Earth-sized Alien World Orbits 'Quiet' Star, Boosting Habitable Potential.Ian O'Neill,How Stuff Works.15 November 2017. Quote:"Tidal lock[ing] is expected for Ross 128 b," says Nicola Astudillo-Defru, who works at the Geneva Observatory, University of Geneva in Switzerland, and is co-author of the study.
  32. ^Ross 128.Sol Station.November 2017.
  33. ^Souto, Diogo; Unterborn, Cayman T.; Smith, Verne V.; Cunha, Katia; Teske, Johanna; Covey, Kevin; Bárbara Rojas-Ayala; García-Hernández, D. A.; Stassun, Keivan (2018)."Stellar and Planetary Characterization of the Ross 128 Exoplanetary System from APOGEE Spectra".The Astrophysical Journal Letters.860(1): L15.arXiv:1805.11633.Bibcode:2018ApJ...860L..15S.doi:10.3847/2041-8213/aac896.hdl:10150/628573.ISSN2041-8205.S2CID89612773.
  34. ^Koren, Marina (July 17, 2017)."The Strange Radio Signals Coming From a Nearby Star – Astronomers have detected a mystery transmission at a frequency they haven't observed before".The Atlantic.RetrievedJuly 17,2017.
  35. ^Shostak, Seth."Signals from A Nearby Star System?".seti.org.Retrieved17 September2017.
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