[edit]Distances of the nearest stars from 20,000 years ago until 80,000 years in the future
This low-mass star has a stellar classification of 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 the infrared band, with the bolometric luminosity being equal to 0.37% of solar.[10] This energy is being radiated from the star's outer atmosphere at an effective temperature of 3,180 K.[4] This gives it the cool orange-red glow of an M-type star.
Ross 128 is an old disk star, which means it has a low abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, and it orbits near the plane of the Milky Way galaxy.[17] The star lacks a strong excess of infrared radiation. An infrared excess is usually an indicator of a dust ring in orbit around the star.[18][19]
Light curves for a flare on FI Virginis, seen in ultraviolet, blue and visual band light, 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 the ultravioletU band, returning to normal brightness in less than an hour. At optical wavelengths, the brightness changes were almost undetectable.[20] It was classified as a flare star and given the variable star designation FI 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 the magnetic braking of 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 the sunspot cycle have 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 an eccentricity of 0.122, causing its distance from the Galactic Center to range between 26.8–34.2 kly (8.2–10.5 kpc).[24] This orbit will bring the star closer to the Solar System in 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]
Ross 128 b was discovered in July 2017 by the HARPS instrument at the La Silla Observatory in Chile, by measuring changes in radial velocity of the host star. Its existence was confirmed on 15 November 2017. It is the second-closest known Earth-size exoplanet, after Proxima 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 likely tidally 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 from APOGEE have 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]
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]
^ 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
^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
^Warren, W. H. Jr. (1978), "Photoelectric Photometric Catalogue of Homogeneous Means in the UBV System", Observatory, Geneva
^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.
^ 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.
^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.
^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
^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
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