Fomalhaut is a young star, for many years thought to be only 100 to 300 million years old, with a potential lifespan of a billion years. MIN M., KAMA M., DOMINIK C. & WATERS L. ADS, A Roadmap to Interstellar Flight & Astrophys., 532, A79 2008 2005 Fomalhaut B (TW Piscis Austrini) is an orange dwarf (K5Vp) that is separated from Fomalhaut A by a distance of 0.91 light years. abstract, Seeing is Believing Rev., 18, 317 SAFFE C., LEVATO H., LOPEZ-GARCIA Z., JOFRE E., PETRUCCI R. & GONZALEZ E. 2016 Suppl., 154, 458 paper, MMT/AO 5 micron Imaging Constraints on the Existence of Giant Planets Orbiting Fomalhaut at ~13-40 AU & BROMLEY B. MNRAS, 406, 1918 Fomalhaut, also called Alpha Piscis Austrini, the 18th star (excluding the Sun) in order of apparent brightness.It is used in navigation because of its conspicuous place in a sky region otherwise lacking in bright stars. MNRAS, 448, 3679 paper, An interferometric study of the Fomalhaut inner debris disk. & Astrophys. 2016 paper  arxiv, Light Scattering and Thermal Emission by Primitive Dust Particles in Planetary Systems Astron. paper, The spin-orbit alignment of the Fomalhaut planetary system probed by optical long baseline interferometry 2013 GRIEßMEIER J.-M., ZARKA P. & SPREEUW H. 2007 KENYON S., CURRIE Th. paper, Long range outward migration of giant planets, with application to Fomalhaut b MARLEY M. LAWLER S., GREENSTREET S. & GLADMAN B. 2010 ACKE B., MIN M., DOMINIK C., VANDENBUSSCHE B., SIBTHORPE B. paper   arxiv, Infrared Non-detection of Fomalhaut b -- Implications for the Planet Interpretation ApJ Letters, 777, L6 2015 Fomalhaut's mass is about 1.92 times that of the Sun, its luminosity is about 16.6 times greater, and its diameter is roughly 1.84 times as large. & Astrophys., 461, 171 ECUVILLON A., ISRAELIAN G., PONT F., SANTOS N. & MAYOR M. MNRAS KASHYAP V., DRAKE J. KENWORTHY M., MESHKAT T., QUANZ S., GIRARD J., MEYER M. & KASPER M. the observed trajectory of Fomalhaut b (Neuh auser et al. The planet will appear to cross a vast belt of debris around the star roughly 20 years from now. Le déplacement de la planète, détectée par le télescope Hubble a permis d'estimer la période de révolution, environ 872 années de terre. ApJ., 646, 505 & Astrophys., 498, L41 paper  arxiv, Signpost of Multiple Planets in Debris Disks The surface temperature of the star is around 8,590 K (8,320 °C). Content and Chapter 5, Are debris disks self-stirred? MAMAJEK E. arxiv, Orbital fitting of imaged planetary companions with high eccentricities and unbound orbits -- Application to Fomalhaut b and PZ Telescopii B & STELL S. paper   astro-ph, The lunar phases of dust grains orbiting Fomalhaut 2004 arxiv, Habitable Zones of Post-Main Sequence Stars 2012 paper  arxiv, Discovery of the Fomalhaut C debris disc 2012 Fomalhaut Luminosity. & Astrophys., 555, A146 ADS, The companion candidate near Fomalhaut - a background neutron star? 2011 GRAHAM J., KALAS P., CHIANG E., FITZGERALD M., CLAMPIN M., KITE E., KRIST J. 2015 paper  arxiv  ADS, Constraining the orbits of sub-stellar companions imaged over short orbital arcs BAAS, 41, no 1, 51.02 Star : Fomalhaut Temperature : 8600 K Radius : 1.85 R ⊙ Age : 100-400 Myr Distance : 7.69 pc 2005 Suspicion (Kalas et al, 2005) Offset of 15 AU + Sharp inner … ApJ, 811, 60 paper, The Ages of Stars Hosting Substellar Companions ApJ., 700, 1647 Astron. & MADDISON S. 2016 BEUST H., BONNEFOY M., MAIRE A.-L., EHRENREICH D., LAGRANGE A.-M. & CHAUNVIN G. Therefore, if Fomalhaut b is a neutron star, it has to be cooler than 91 000 K and closer than 13.5 pc. Fomalhaut has a spectral type of A3V, a surface temperature of 8750° Kelvin and a luminosity 17.9 times the Sun. 2013 MNRAS, in press 2012 KENYON, S. & B. BROMLEY ApJ., 625, 390, A planetary system as the origin of structure in Fomalhaut's dust belt. Science, 322, 1335 Astron. Letters, 702, L158 Ann. Astron. & MOORE A. NEUHAUSER R. & SCHMIDT T. DELLER A. 2013 Constraining the Planetary System of Fomalhaut Using High-Resolution ALMA Observations 2015 Fomalhaut b was first described in 2008 by Paul Kalas, James Graham and colleagues at the University of California, Berkeley. Astron. Display orbital revolution of Fomalhaut b around the hoststar Fomalhaut, http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Fomalhaut+&submit=SIMBAD+search, http://www.openexoplanetcatalogue.com/planet/Fomalhaut%20b/, Semi Major Axis / Orbital Distance Calculated. ApJ., 649, 1010 2009 paper, Extrasolar planet taxonomy: a new statistical approach The observations include the discoveries of tenuous nebulosity beyond the main dust belt detected to at least 209 AU projected radius, and a ~50 AU wide azimuthal gap in the belt northward of Fomalhaut b. STAPELFELDT K., HOLMES E., CHEN C., RIEKE G., SU K., HINES D., WERNER M., BEICHMAN C., JURA M., PADGETT D., STANSBERRY J., BENDO G., CADIEN J., MARENGO M., THOMPSON T., VELUSAMY T., BACKUS C., BLAYLOCK M., EGAMI E., ENGELBRECHT C., FRAYER D., GORDON K., KEENE J., LATTER W., MEGEATH T., MISSELT K., MORRISON J., MUZEROLLE J., NORIEGA-CRESPO A., Van CLEVE J. CHIANG E., KITE E., KALAS P., GRAHAM J. KALAS P., GRAHAM J., FITZGERALD M. & CLAMPIN M. paper, Analysis of the Photometry of Fomalhaut b NORDSTROM B., MAYOR M., ANDERSEN J., HOLMBERG J., PONT F., JORGENSEN B., OLSEN E., UDRY S. & MOWLAVI N. ApJ Letters, 760, L32 Planetary system ? 2009 We present new optical coronagraphic data of Fomalhaut obtained with HST/STIS in 2010 and 2012.Fomalhaut b is recovered at both epochs to high significance. paper, Giant Planet Formation Conference: American Astronomical Society Meeting Abstracts #213; Authors: Phil Kalas Nature, 405, 1067 MacGREGOR M., WILNER D., CHANDLER C., RICCI L., MADDISON S. et al. ApJ., 582, 5821141 CRIDA A., MASSET F. & MORBIDELLI A. $ Tel, Fomalhaut, g Lup, HD181327 and HR8799 & Astrophys., 574, L1 & MEGEATH S. ApJ, 764, 7 2009 We consider the ability of three models—impacts, captures, and collisional cascades—to account for a bright cloud of dust in Fomalhaut b. 2013 2008 abstract, Fomalhaut b: Direct Detection of a less than 3 Jupiter-mass Object Orbiting Fomalhaut arxiv   & HINKLEY S. SCHMIDT T., NEUHÄUSER R. & SEIFAHRT A. & STAPELFELDT K. Astron. abstract, The Hill stability of the possible moons of extrasolar planets paper   arxiv, Fomalhaut debris disk emission at 7 millimeters: constraints on the collisional models of planetesimals & AMARAA. 2015 (cf. LEBRETON J., van LIESHOUT R., AUGEREAU J.-Ch., ABSIL O., MENNESSON B. ApJ. Substellar companion NAME Fomalhaut b detected, see Fomalhaut in the Extrasolar Planets Encyclopaedia. 2012 paper  arxiv, Constraints on the gas content of the Fomalhaut debris belt; Can gas-dust interactions explain the belt's morphology? ApJ, 763, 119 paper, Submillimeter Observations of an Asymmetric Dust Disk Astron. ApJ. Habitability by Solar Eq. in IAU Symposium No. 2013), and in addition hosts an enigmatic exoplanet, Fomalhaut b (Kalas et … Method and first results MESHKAT T., KENWORTHY M., QUANZS. 22{25 mag, depending on temperature (Kaplan et al. Astronomical Unit: Hubble Space Telescope Guide Star Catalog (GSC) ID, "Paul Kalas, James R. Graham, Michael P. Fitzgerald, Mark Clampin", STIS Coronagraphic Imaging of Fomalhaut: Main Belt Structure and the Orbit of Fomalhaut b. arxiv, Constraints on Planetesimal Collision Models in Debris Disks It lies in the southern constellation Piscis Austrinus, 25 light-years from Earth.A white star, it has an apparent magnitude of 1.16. Our analysis is based on a novel approach to the power-law size distribution of solid particles central to each model. Astron. around Fomalhaut. paper, Homogeneous comparison of planet candidates imaged directly until 2008 Ann. A 2012 study gave a slightly higher age of 440 ± 40 million years. Arcturus A star that is a little more massive than the sun but with 25 times the sun’s radius, Arcturus is ascending the red-giant branch of the Hertzsprung-Russell diagram. Astrobiology, 12, 361 2016 paper   arxiv   ADS, Kinematics of planet-host stars and their relation to dynamical streams in the solar neighbourhood SU K. & RIEKE G. Astron. 2016 MARCHI S. 2006 RICCI L., TESTI L., MADDISON S. & WILNER D. paper, Spitzer/Infrared Array Camera Limits to Planetary Companions of Fomalhaut and epsilon Eridani Son existence avait été prédite, dès 2006, par Alice C. Quillen [7]. Fomalhaut b was first described in 2008 by Paul Kalas, James Graham and colleagues at the University of California, Berkeley. & LEBRETON J. Science, 322, 1345 & Astrophys., 419, 989 2011 PLAVALOVA E. from its host star. Luminosity is the amount of energy that a star pumps out and its relative to the amount that our star, the Sun gives out. 2010 ApJ. paper   arxiv, An interferometric study of the Fomalhaut inner debris disk II. paper, Numerical Modelling of Dusty Debris Disks. LEE E. & CHAING E. Letters, 754, L20 paper, Catalog of Nearby Exoplanets It has a mass of 2.1 solar masses and a diameter 1.8 times the Sun. & 4 additional authors 2009 2015 2010 ApJ, accepted KIMURA H., KOLOKOLOVA L. LI A. J., submitted paper  arxiv, A Deep Keck/NIRC2 Search for Thermal Emission from Planetary Companions Orbiting Fomalhaut paper   arxiv, Direct Imaging of Extra-solar Planets - Homogeneous Comparison of Detected Planets and Candidates 2007 NERO D. & BJORKMAN E. SCHNEIDER J., DEDIEU C., LE SIDANER P., SAVALLE R. & ZOLOTUKHIN I. 2006 2010 arxiv, Collisional Cascade Calculations for Irregular Satellite Swarms in Fomalhaut b arxiv   Astron. The companions are loosely bound to the primary star; B is 58,000 AU (0.28 parsecs) from Fomalhaut and C is 158,000 AU (0.77 parsecs) away. abstract   Jako infracrveno zračenje i posjeduje nekoliko cirkumstelarnih omotača C., DENT W. et al was described... Fomalhaut is 25.04 light years away from the Sun Optical to Submillimeter of... Astronomy 2009 OPPENHEIMER b 22 { 25 mag, depending on temperature ( et. Asteroid and Kuiper belts ( Su et al G dwarfs a star exhibiting variations luminosity! 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