Because of Proxima Centauri's proximity to Earth, its angular diameter can be measured directly. The star is about one-seventh the actual diameter of the Sun. It has a mass about an eighth of the Sun's mass (M☉), and its average density is about 33 times that of the Sun.[nb 3] Although it has a very low average luminosity, Proxima is a flare star that undergoes random dramatic increases in brightness because of magnetic activity. The star's magnetic field is created by convection throughout the stellar body, and the resulting flare activity generates a total X-ray emission similar to that produced by the Sun. The mixing of the fuel at Proxima Centauri's core through convection and its relatively low energy-production rate mean that it will be a main-sequence star for another four trillion years, or nearly 300 times the current age of the universe.
In 2016, the European Southern Observatory announced the discovery of Proxima b, a planet orbiting the star at a distance of roughly 0.05AU (7.5millionkm) with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.3 times that of the Earth. The equilibrium temperature of Proxima b is estimated to be within the range of where water could exist as liquid on its surface, thus placing it within the habitable zone of Proxima Centauri, although because Proxima Centauri is a red dwarf and a flare star, whether it could support life is disputed. Previous searches for orbiting companions had ruled out the presence of brown dwarfs and supermassive planets.
In 1951, American astronomer Harlow Shapley announced that Proxima Centauri is a flare star. Examination of past photographic records showed that the star displayed a measurable increase in magnitude on about 8% of the images, making it the most active flare star then known. The proximity of the star allows for detailed observation of its flare activity. In 1980, the Einstein Observatory produced a detailed X-ray energy curve of a stellar flare on Proxima Centauri. Further observations of flare activity were made with the EXOSAT and ROSATsatellites, and the X-ray emissions of smaller, solar-like flares were observed by the Japanese ASCA satellite in 1995. Proxima Centauri has since been the subject of study by most X-ray observatories, including XMM-Newton and Chandra.
Because of Proxima Centauri's southern declination, it can only be viewed south of latitude27°N.[nb 4] Red dwarfs such as Proxima Centauri are far too faint to be seen with the naked eye. Even from Alpha Centauri A or B, Proxima would only be seen as a fifth magnitude star. It has an apparent visual magnitude of 11, so a telescope with an aperture of at least 8cm (3.1in) is needed to observe it, even under ideal viewing conditions—under clear, dark skies with Proxima Centauri well above the horizon.
The two bright points are the Alpha Centauri system (left) and Beta Centauri (right). The faint red star in the centre of the red circle is Proxima Centauri.
In 2002, optical interferometry with the Very Large Telescope (VLTI) found that the angular diameter of Proxima Centauri was 6991494509954731727♠1.02±0.08mas. Because its distance is known, the actual diameter of Proxima Centauri can be calculated to be about 1/7 that of the Sun, or 1.5 times that of Jupiter. The star's estimated mass is 12.2%M☉, or 129 Jupiter masses (MJ). The mean density of main-sequence stars increase with decreasing mass, and Proxima Centauri is no exception: it has a mean density of 47.1×103kg/m3 (47.1g/cm3), compared with the Sun's mean density of 1.411×103kg/m3 (1.411g/cm3).[nb 3]
A 1998 study of photometric variations indicates that Proxima Centauri rotates once every 83.5 days. A subsequent time series analysis of chromospheric indicators in 2002 suggests a longer rotation period of 7002116600000000000♠116.6±0.7days. This was subsequently ruled out in favor of a rotation period of 7001826000000000000♠82.6±0.1days.
Because of its low mass, the interior of the star is completely convective, causing energy to be transferred to the exterior by the physical movement of plasma rather than through radiative processes. This convection means that the helium ash left over from the thermonuclear fusion of hydrogen does not accumulate at the core, but is instead circulated throughout the star. Unlike the Sun, which will only burn through about 10% of its total hydrogen supply before leaving the main sequence, Proxima Centauri will consume nearly all of its fuel before the fusion of hydrogen comes to an end.
Convection is associated with the generation and persistence of a magnetic field. The magnetic energy from this field is released at the surface through stellar flares that briefly increase the overall luminosity of the star. These flares can grow as large as the star and reach temperatures measured as high as 27million K—hot enough to radiate X-rays. Proxima Centauri's quiescent X-ray luminosity, approximately (4–16)×1026erg/s ((4–16)×1019W), is roughly equal to that of the much larger Sun. The peak X-ray luminosity of the largest flares can reach 1028erg/s (1021W).
Proxima Centauri's chromosphere is active, and its spectrum displays a strong emission line of singly ionized magnesium at a wavelength of 280nm. About 88% of the surface of Proxima Centauri may be active, a percentage that is much higher than that of the Sun even at the peak of the solar cycle. Even during quiescent periods with few or no flares, this activity increases the corona temperature of Proxima Centauri to 3.5million K, compared to the 2million K of the Sun's corona. Proxima Centauri's overall activity level is considered low compared to other red dwarfs, which is consistent with the star's estimated age of 4.85×109years, since the activity level of a red dwarf is expected to steadily wane over billions of years as its stellar rotation rate decreases. The activity level also appears to vary with a period of roughly 442 days, which is shorter than the solar cycle of 11 years.
Proxima Centauri has a relatively weak stellar wind, no more than 20% of the mass loss rate of the solar wind. Because the star is much smaller than the Sun, the mass loss per unit surface area from Proxima Centauri may be eight times that from the solar surface.
A red dwarf with the mass of Proxima Centauri will remain on the main sequence for about four trillion years. As the proportion of helium increases because of hydrogen fusion, the star will become smaller and hotter, gradually transforming from red to blue. Near the end of this period it will become significantly more luminous, reaching 2.5% of the Sun's luminosity (L☉) and warming up any orbiting bodies for a period of several billion years. When the hydrogen fuel is exhausted, Proxima Centauri will then evolve into a white dwarf (without passing through the red giant phase) and steadily lose any remaining heat energy.
Among the known stars, Proxima Centauri has been the closest star to the Sun for about 32,000years and will be so for about another 25,000years, after which Alpha Centauri A and Alpha Centauri B will alternate approximately every 79.91 years as the closest star to the Sun. In 2001, J. García-Sánchez et al. predicted that Proxima will make its closest approach to the Sun in approximately 26,700years, coming within 3.11ly (0.95pc). A 2010 study by V. V. Bobylev predicted a closest approach distance of 2.90ly (0.89pc) in about 27,400years, followed by a 2014 study by C. A. L. Bailer-Jones predicting a perihelion approach of 3.07ly (0.94pc) in roughly 26,710years. Proxima Centauri is orbiting through the Milky Way at a distance from the Galactic Centre that varies from 27 to 31kly (8.3 to 9.5kpc), with an orbital eccentricity of 0.07.
Ever since the discovery of Proxima, it has been suspected to be a true companion of the Alpha Centauri binary star system. Data from the Hipparcos satellite, combined with ground-based observations, were consistent with the hypothesis that the three stars are a bound system. For this reason, Proxima is sometimes referred to as Alpha CentauriC. Kervella et al. (2017) used high-precision radial velocity measurements to determine with a high degree of confidence that Proxima and Alpha Centauri are gravitationally bound. Proxima's orbital period around the Alpha CentauriAB barycenter is 7005547000000000000♠547000+6600 −4000 years with an eccentricity of 6999500000000000000♠0.5±0.08; it approaches Alpha Centauri to 7014643270844010000♠4300+1100 −900AU at periastron and retreats to 7015194477231910000♠13000+300 −100AU at apastron. At present, Proxima is 12,947±260AU (1.94±0.04trillionkm) from the Alpha CentauriAB barycenter, nearly to the farthest point in its orbit.
Such a triple system can form naturally through a low-mass star being dynamically captured by a more massive binary of 1.5–2M☉ within their embedded star cluster before the cluster disperses. However, more accurate measurements of the radial velocity are needed to confirm this hypothesis. If Proxima was bound to the Alpha Centauri system during its formation, the stars are likely to share the same elemental composition. The gravitational influence of Proxima might also have stirred up the Alpha Centauri protoplanetary disks. This would have increased the delivery of volatiles such as water to the dry inner regions, so possibly enriching any terrestrial planets in the system with this material. Alternatively, Proxima may have been captured at a later date during an encounter, resulting in a highly eccentric orbit that was then stabilized by the Galactic tide and additional stellar encounters. Such a scenario may mean that Proxima's planetary companion has had a much lower chance for orbital disruption by Alpha Centauri.
Six single stars, two binary star systems, and a triple star share a common motion through space with Proxima Centauri and the Alpha Centauri system. The space velocities of these stars are all within 10km/s of Alpha Centauri's peculiar motion. Thus, they may form a moving group of stars, which would indicate a common point of origin, such as in a star cluster.
Though Proxima Centauri is the nearest bona fide star, it is still possible that one or more as-yet undetected sub-stellar brown dwarfs may lie closer.
Proxima Centaurib is a planet orbiting the star at a distance of roughly 0.05AU (7.5millionkm) with an orbital period of approximately 11.2 Earth days. Its estimated mass is at least 1.3 times that of the Earth. Moreover, the equilibrium temperature of Proximab is estimated to be within the range where water could exist as liquid on its surface; thus, placing it within the habitable zone of Proxima Centauri.
A second signal in the range of 60 to 500 days was also detected, but its nature is still unclear due to stellar activity.
Prior to this discovery, multiple measurements of the star's radial velocity constrained the maximum mass that a detectable companion to Proxima Centauri could possess. The activity level of the star adds noise to the radial velocity measurements, complicating detection of a companion using this method. In 1998, an examination of Proxima Centauri using the Faint Object Spectrograph on board the Hubble Space Telescope appeared to show evidence of a companion orbiting at a distance of about 0.5AU. A subsequent search using the Wide Field Planetary Camera 2 failed to locate any companions.Astrometric measurements at the Cerro Tololo Inter-American Observatory appear to rule out a Jovian companion with an orbital period of 2−12years.
Proxima Centauri, along with Alpha CentauriA andB, was among the "Tier1" target stars for NASA's now-canceled Space Interferometry Mission (SIM), which would theoretically have been able to detect planets as small as three Earth masses (M⊕) within two AU of a "Tier1" target star.
In 2017, a team of astronomers using the Atacama Large Millimeter/submillimeter Array reported detecting a belt of dust orbiting Proxima Centauri at a range of 1−4AU from the star. This dust has a temperature of around 40K and has a total estimated mass of 1% of the planet Earth. They also tentatively detected two additional features: a cold belt with a temperature of 10K orbiting around 30AU and a compact emission source about 1.2arcseconds from the star. However, upon further analysis, these emissions were determined to be the result of a large flare emitted by the star in March, 2017. The presence of dust is not needed to model the observations.
Prior to the discovery of Proxima Centauri b, the TV documentary Alien Worlds hypothesized that a life-sustaining planet could exist in orbit around Proxima Centauri or other red dwarfs. Such a planet would lie within the habitable zone of Proxima Centauri, about 0.023–0.054AU (3.4–8.1millionkm) from the star, and would have an orbital period of 3.6–14days. A planet orbiting within this zone may experience tidal locking to the star. If the orbital eccentricity of this hypothetical planet is low, Proxima Centauri would move little in the planet's sky, and most of the surface would experience either day or night perpetually. The presence of an atmosphere could serve to redistribute the energy from the star-lit side to the far side of the planet.
Proxima Centauri's flare outbursts could erode the atmosphere of any planet in its habitable zone, but the documentary's scientists thought that this obstacle could be overcome. Gibor Basri of the University of California, Berkeley, mentioned that "no one [has] found any showstoppers to habitability". For example, one concern was that the torrents of charged particles from the star's flares could strip the atmosphere off any nearby planet. If the planet had a strong magnetic field, the field would deflect the particles from the atmosphere; even the slow rotation of a tidally locked planet that spins once for every time it orbits its star would be enough to generate a magnetic field, as long as part of the planet's interior remained molten.
Because of the star's proximity to Earth, Proxima Centauri has been proposed as a flyby destination for interstellar travel. Proxima currently moves toward Earth at a rate of 22.2km/s. After 26,700 years, when it will come within 3.11light-years, it will begin to move farther away.
If non-nuclear, conventional propulsion technologies are used, the flight of a spacecraft to a planet orbiting Proxima Centauri would probably require thousands of years. For example, Voyager 1, which is now travelling 17km/s (38,000mph) relative to the Sun, would reach Proxima in 73,775 years, were the spacecraft travelling in the direction of that star. A slow-moving probe would have only several tens of thousands of years to catch Proxima Centauri near its closest approach, and could end up watching it recede into the distance.
Project Breakthrough Starshot aims to reach the Alpha Centauri system within the first half of the 21st century, with microprobes travelling at twenty percent of the speed of light propelled by around 100 gigawatts of Earth-based lasers. The probes will perform a fly-by of Proxima Centauri to take photos and collect data of its planet's atmospheric composition. It will take 4.22 years for the information collected to be sent back to Earth.
From Proxima Centauri, the Sun would appear as a bright 0.4-magnitude star in the constellation Cassiopeia.[nb 8]
1 2 The density (ρ) is given by the mass divided by the volume. Relative to the Sun, therefore, the density is:
= 0.122 · 0.154−3 · (1.41×103kg/m3)
= 33.4 · (1.41×103kg/m3)
where is the average solar density. See:
Munsell, Kirk; Smith, Harman; Davis, Phil; Harvey, Samantha (June 11, 2008). "Sun: facts & figures". Solar system exploration. NASA. Archived from the original on January 2, 2008. Retrieved July 12, 2008.
Bergman, Marcel W.; Clark, T. Alan; Wilson, William J. F. (2007). Observing projects using Starry Night Enthusiast (8th ed.). Macmillan. pp.220–221. ISBN1-4292-0074-X.
↑ For a star south of the zenith, the angle to the zenith is equal to the Latitude minus the Declination. The star is hidden from sight when the zenith angle is 90° or more, i.e. below the horizon. Thus, for Proxima Centauri:
↑ This is actually an upper limit on the quantity m sin i, where i is the angle between the orbit normal and the line of sight, in a circular orbit. If the planetary orbits are close to face-on as observed from Earth, or in an eccentric orbit, more massive planets could have evaded detection by the radial velocity method.
↑ The coordinates of the Sun would be diametrically opposite Proxima, at α=02h29m42.9487s, δ=+62°40′46.141″. The absolute magnitude Mv of the Sun is 4.83, so at a parallax π of 0.77199 the apparent magnitude m is given by 4.83 − 5(log10(0.77199) + 1) = 0.40. See: Tayler, Roger John (1994). The Stars: Their Structure and Evolution. Cambridge University Press. p.16. ISBN0-521-45885-4.
1 2 3 Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E. L.; Kirkpatrick, J. D.; Light, R. M.; Marsh, K. A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W. A.; Wheelock, S.; Zacarias, N. (2003). "VizieR online data catalog: 2MASS all-sky catalog of point sources (Cutri+ 2003)". VizieR on-line data catalog: II/246. Originally published in: 2003yCat.2246....0C. 2246: 0. Bibcode:2003yCat.2246....0C.
↑ 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.
1 2 3 Benedict, G. Fritz, Chappell DW, Nelan E, Jefferys WH, Van Altena W, Lee J, Cornell D, Shelus PJ (1999). "Interferometric astrometry of Proxima Centauri and Barnard's Star using Hubble Space Telescope fine guidance sensor 3: detection limits for substellar companions". The Astronomical Journal. 118 (2): 1086–1100. arXiv:astro-ph/9905318. Bibcode:1999AJ....118.1086B. doi:10.1086/300975.
1 2 See Table 1, Doyle, J. G.; Butler, C. J. (1990). "Optical and infrared photometry of dwarf M and K stars". Astronomy and Astrophysics. 235: 335–339. Bibcode:1990A&A...235..335D. and p. 57, Peebles, P. J. E. (1993). Principles of physical cosmology. Princeton, New Jersey: Princeton University Press. ISBN0-691-01933-9.
↑ Christian, D. J.; Mathioudakis, M.; Bloomfield, D. S.; Dupuis, J.; Keenan, F. P. (2004). "A detailed study of opacity in the upper atmosphere of Proxima Centauri". The Astrophysical Journal. 612 (2): 1140–1146. Bibcode:2004ApJ...612.1140C. doi:10.1086/422803.
1 2 Khodachenko, Maxim L., Lammer H, Grießmeier J, Leitner M, Selsis F, Eiroa C, Hanslmeier A, Biernat HK (2007). "Coronal Mass Ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. I. CME impact on expected magnetospheres of earth-like exoplanets in close-in habitable zones". Astrobiology. 7 (1): 167–184. Bibcode:2007AsBio...7..167K. doi:10.1089/ast.2006.0127. PMID17407406.
1 2 Kürster, M.; Hatzes, A. P.; Cochran, W. D.; Döbereiner, S.; Dennerl, K.; Endl, M. (1999). "Precise radial velocities of Proxima Centauri. Strong constraints on a substellar companion". Astronomy & Astrophysics Letters. 344: L5–L8. arXiv:astro-ph/9903010. Bibcode:1999A&A...344L...5K.
1 2 Schroeder, Daniel J.; Golimowski, David A.; Brukardt, Ryan A.; Burrows, Christopher J.; Caldwell, John J.; Fastie, William G.; Ford, Holland C.; Hesman, Brigette; Kletskin, Ilona; Krist, John E.; Royle, Patricia; Zubrowski, Richard. A. (2000). "A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2". The Astronomical Journal. 119 (2): 906–922. Bibcode:2000AJ....119..906S. doi:10.1086/301227.
↑ Innes, R. T. A. (October 1915). "A Faint Star of Large Proper Motion". Circular of the Union Observatory Johannesburg. 30: 235–236. Bibcode:1915CiUO...30..235I. This is the original Proxima Centauri discovery paper.
↑ Innes, R. T. A. (September 1917). "Parallax of the Faint Proper Motion Star Near Alpha of Centaurus. 1900. R.A. 14 h 22m 55s.-0s 6t. Dec-62° 15'2 0'8 t". Circular of the Union Observatory Johannesburg. 40: 331–336. Bibcode:1917CiUO...40..331I.
↑ Zombeck, Martin V. (2007). Handbook of space astronomy and astrophysics (Third ed.). Cambridge, UK: Cambridge University Press. p.109. ISBN0-521-78242-2.
↑ Benedict, G. F., McArthur, B., Nelan E, Story D, Whipple AL, Shelus PJ, Jefferys WH, Hemenway PD, Franz OG (1998). "Photometry of Proxima Centauri and Barnard's Star using Hubble Space Telescope fine guidance sensor 3: a search for periodic variations". The Astronomical Journal. 116 (1): 429–439. arXiv:astro-ph/9806276. Bibcode:1998AJ....116..429B. doi:10.1086/300420.
↑ Suárez Mascareño, A.; Rebolo, R.; González Hernández, J. I.; Esposito, M. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441.
↑ Stauffer, J. R.; Hartmann, L. W. (1986). "Chromospheric activity, kinematics, and metallicities of nearby M dwarfs". Astrophysical Journal Supplement Series. 61 (2): 531–568. Bibcode:1986ApJS...61..531S. doi:10.1086/191123.
↑ Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; Hoeg, E.; Bastian, U.; Bernacca, P. L.; Crézé, M.; Donati, F.; Grenon, M.; Grewing, M.; van Leeuwen, F.; van der Marel, H.; Mignard, F.; Murray, C. A.; Le Poole, R. S.; Schrijver, H.; Turon, C.; Arenou, F.; Froeschlé, M.; Petersen, C. S. (July 1997), "The Hipparcos catalogue", Astronomy and Astrophysics, 323: L49–L52, Bibcode:1997A&A...323L..49P.
↑ Schultz, A. B.; Hart, H. M.; Hershey, J. L.; Hamilton, F. C.; Kochte, M.; Bruhweiler, F. C.; Benedict, G. F.; Caldwell, John; Cunningham, C.; Wu, Nailong; Franz, O. G.; Keyes, C. D.; Brandt, J. C. (1998). "A possible companion to Proxima Centauri". Astronomical Journal. 115 (1): 345–350. Bibcode:1998AJ....115..345S. doi:10.1086/300176.
↑ Lurie, John C.; Henry, Todd J.; Jao, Wei-Chun; Quinn, Samuel N.; Winters, Jennifer G.; Ianna, Philip A.; Koerner, David W.; Riedel, Adric R.; Subasavage, John P. (November 2014). "The Solar Neighborhood. XXXIV. a Search for Planets Orbiting Nearby M Dwarfs Using Astrometry". The Astronomical Journal. 148 (5): 12. arXiv:1407.4820. Bibcode:2014AJ....148...91L. doi:10.1088/0004-6256/148/5/91. 91.
↑ Endl, M.; Kuerster, M.; Rouesnel, F.; Els, S.; Hatzes, A. P.; Cochran, W. D. (June 18–21, 2002). Deming, Drake, ed. Extrasolar terrestrial planets: can we detect them already?. Conference Proceedings, Scientific Frontiers in Research on Extrasolar Planets. Washington, DC. pp.75–79. arXiv:astro-ph/0208462. Bibcode:2003ASPC..294...75E.