December 1, 2020

Astron. & MARSHALL J. 2011 It was obtained with the Keck II telescope on Hawaii. 2010 [24] If the mass estimates are correct, the HR 8799 system is the first multiple-planet extrasolar system to be directly imaged. ApJ., 710, 1375 The broadband photometry of planets b, c and d has shown that there may be significant clouds in their atmospheres,[22] while the infrared spectroscopy of planets b and c pointed to non-equilibrium CO/CH4 chemistry. arxiv, A Combined Subaru/VLT/MMT 1-5 μm Study of Planets Orbiting HR 8799: Implications for Atmospheric Properties, Masses, and Formation A csillag körül porkorongot is találtak, kijjebb, 75 CsE távolságra. Query : HR 8799 : C.D.S. & Astrophys., 528, A134 In January 2009 the Spitzer Space Telescope obtained images of the debris disk around HR 8799. PASP, 128, 102001 The implications of the simultaneous spectra of all four planets obtained with Project 1640 are summarized as follows: Planet b contains ammonia and/or acetylene as well as carbon dioxide, but has little methane; Planet c contains ammonia, perhaps some acetylene but neither carbon dioxide nor substantial methane; Planet d contains acetylene, methane, and carbon dioxide but ammonia is not definitively detected; Planet e contains methane and acetylene but no ammonia or carbon dioxide. PETIT dit de la ROCHE D., van den ANKER M., KISSLER-PATIG M., IVANOV V. & FEDELE D. 2011 & Astrophys., 587, A57 The first spectroscopic study of planet b (performed at near-infrared wavelengths) detected strong water absorption, which indicates a hydrogen-rich atmosphere. 2011 paper, Orbital Properties of the HR 8799 Planetary System Content and Chapter 5, Adaptive Optics Observations of Exoplanets, Brown Dwarfs, & Binary Stars paper, High-Contrast Observations in Optical and Infrared Astronomy paper   arxiv, Resolved Submillimeter Observations of the HR 8799 and HD 107146 Debris Disks SCHMIDT T., NEUHÄUSER R. & SEIFAHRT A. {\displaystyle \scriptstyle {\sqrt {4.9}}} SPIE Optics+Photonics paper  arxiv, Resolved Millimeter Observations of the HR 8799 Debris Disk Those planets, along with Fomalhaut b, were the first exoplanets whose orbital motion was confirmed by direct imaging. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same data set. 2011 & MAROIS Ch. ADS, Towards a dynamics-based estimate of the extent of HR 8799's unresolved warm debris belt BOWLER B. [23], The outer planet orbits inside a dusty disk like the Solar Kuiper belt. & SIEGLER N. This page was last edited on 17 November 2020, at 18:26. & Astrophys., 598, A83 GAUDI, B., SEAGER, S. MENNESSON, B., KIESSLING, A., WARFIELD, K. et al. 2016 & Astrophys., submitted GERARD B., LAWLER S., MAROIS Ch., TANNOCK M., MATTHEWS B. The temperature of the stellar corona is about 3.0 million K.[13], On 13 November 2008, Christian Marois of the National Research Council of Canada's Herzberg Institute of Astrophysics and his team announced they had directly observed three planets orbiting the star with the Keck and Gemini telescopes in Hawaii,[17][18][19][20] in both cases employing adaptive optics to make observations in the infrared. CRILL B. Media in category "HR 8799 d" The following 5 files are in this category, out of 5 total. paper   The star HR 8799 is a member of the Lambda Boötis (λ Boo) class, a group of peculiar stars with an unusual lack of metals—elements heavier than hydrogen and helium—in their upper atmosphere. [25], A number of studies have used the spectra of HR 8799's planets to determine their chemical compositions and constrain their formation scenarios. abstract, Direct imaging of extrasolar planets: overview of ground and space programs Compared to models of planetary atmospheres, this first spectrum of planet b is best matched by a model of enhanced metallicity (about 10 times the metallicity of the Sun), which may support the notion that this planet formed through core-accretion. 2020 A larger sample from photometric distances At around the same time, a … HR 8799 is ’n hoofreeksster van rofweg 30 miljoen jaar oud sowat 129 ligjare van die Aarde af in die sterrebeeld Vlieënde Perd.Sy massa is rofweg 1,5 keer dié van die Son en sy ligsterkte 4,9 keer die Son s'n. The brightest body in the constellation Piscis Austrinus is Fomalhaut. paper, An image of an exoplanet separated by two diffraction beamwidths from a star arxiv  2016 Yes, we are in the era of watching planets orbit other stars. hr 8799 is a collection of spatial compositions: hr 8799 a, hr 8799 b, hr 8799 c, hr 8799 d. They can be presented in various media such as on paper, in videos or as a metallic sculpture. [26], The first simultaneous spectra of all four known planets in the HR 8799 system were obtained in 2012 using the Project 1640 instrument at Palomar Observatory. KALAS P., FITZGERALD M., PAPADOPOULOS P., GRAHAM J., MANESS H., MATTHEWS B., CLAMPIN M., CHIANG E. & BASU K. [37], Media related to HR 8799 at Wikimedia Commons, Coordinates: 23h 07m 28.7150s, +21° 08′ 03.302″, Vortex Coronagraph: Testbed for high-contrast imaging technology, The planets are young and therefore they are still hot and bright in the, Centre de données astronomiques de Strasbourg, "HR 8799: A Link between γ Doradus Variables and λ Bootis Stars", Monthly Notices of the Royal Astronomical Society: Letters, "λ Bootis-Like Abundances in the Vega-Like, γ Doradus Type-Pulsator HD 218396", "First direct detection of an exoplanet by optical interferometry. 2012 2012 2010 & HINKLEY S. 2015 paper   CLOSE L. & MALES J. & Astrophys. in "14th Australian Space Research Conference" The HR 8799 planetary system is the first solar system beyond our own that astronomers directly imaged. All of her planets have up to 4 Jupiter masses, which make them very massive planets. SPIE Astronomical Telescopes and Instrumentation HINKLEY S., CARPENTER J. ApJ, accepted lació de Pegàs. SODOR A., CHENE A.-N., DE CAT P., BOGNAR Zs., WRIGHT D. et al. APAI D., KASPER M., SKEMER A., HANSON J., LAGRANGE A.-M. et al. ApJ., 741, 55 paper   arxiv, High-Mass, Four-Planet Models for HR 8799: Constraining the Orbital Inclination and Age of the System The star's name of HR 8799 is the designation that it has as its identifier in the Bright Star Catalogue. HR 8799 is a roughly 30 million-year-old main-sequence star located 129 light years (39 parsecs) away from Earth in the constellation of Pegasus. 2010 Icarus, 207, 503 [36] In 2011, three further exoplanets were rendered viewable in a NICMOS image taken in 1998, using advanced data processing. It is part of a system that also contains a debris disk and at least four massive planets. Because of the inverse square law relating radiation intensity to distance from the source, comparable radiation intensities are present at distances MARLEY M., SAUMON D., CUSHING M., ACKERMAN A., FORTNEY J. & Astrophys., accepted New spectrophotometry and astrometry of the HR 8799 exoplanetary system De magnitud aparent mitjana +5,96, es troba a 129 anys llum de distància del sistema solar. 2010 More accurately, asteroseismology also suggests an age of approximately a billion years. CURRIE Th., BURROWS A., GIRARD J., CLOUTIER R., FUKAGAWA M. et al. ApJ., 716, 417 CURIE Th., GUYON O., LOZI J., GROFF T., KASDIN J. et al. 2014 It has a 5.96 magnitude and it is located inside the western edge of the great square of Pegasus almost exactly halfway between Scheat and Markab. Specifically, it is easier to obtain images when the planet is especially large (considerably larger than Jupiter), widely separated from its parent star, and hot so that it emits intense infrared radiation. paper, Stable Four-Planet Configurations for HR8799 abstract, Did Fomalhaut, HR 8799, and HL Tauri Form Planets via the Gravitational Instability? 2014 ADS, Imaging Extrasolar Giant Planets ADS, VLT/SPHERE robust astrometry of the HR8799 planets at milliarcsecond-level accuracy Orbital architecture analysis with PyAstrOFit in "Origins 2014" conference (Nara, Japan paper   ADS, HR 8799: The Benchmark Directly-Imaged Planetary System arxiv, VLT/SPHERE robust astrometry of the HR8799 planets at milliarcsecond-level accuracy Orbital architecture analysis with PyAstrOFit PEARCE T., WYATT M. & KENNEDY G. GEILER F., KRIKOV A., BOOTH M. & LÖNE T. paper   astro-ph, Stability of the directly imaged multiplanet system HR 8799: resonance and masses [17] The system is more likely to be stable if the planets "e", "d" and "c" are in a 4:2:1 resonance, which would imply that the orbit of the planet d has an eccentricity exceeding 0.04 in order to match the observational constraints. preprint, Multiple Planets Orbiting the Star HR 8799 MOYA A. RAMOS X., CHRALAMBOUS C., BENITEZ-LlAMBAY P. & BEAUGE C. paper   Science. These objects are near the upper mass limit for classification as planets; if they exceeded 13 Jupiter masses, they would be capable of deuterium fusion in their interiors and thus qualify as brown dwarfs under the definition of these terms used by the IAU's Working Group on Extrasolar Planets. arxiv  2010 λ Boötis stars like this are generally young, with a mean age of a billion years. 2009 2009 abstract, Planet Formation at Wide Separations: Constraints from HR 8799 Astron. & VENN K. 2009 & Astrophys., 638, A50 & FREEDMAN R. HINKLEY S., CARPENTER J., IRELAND M. & KRAUS A. MARLEY M. Astron. paper  arxiv  ADS, Exoplanetary Atmospheres - Chemistry, Formation Conditions, and Habitability paper, Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs FABRYCKY D. & MURRAY-CLAY R. 2011 paper, Non-redundant Aperture Masking Constraints on Massive Companions within 12 AU of the HR 8799 System DONNISON J. 2019 & MAROIS Ch. MNRAS, 156, 276 Astron. paper   arxiv, Pulsating stars harbouring planets & ACEITUNO F. Astron. [8] However, this is disputed because it would make the planets become brown dwarfs to fit into the cooling models. Rev., accepted MERU F. & BATE M. Three components of the debris disk were distinguished: The halo is unusual and implies a high level of dynamic activity which is likely due to gravitational stirring by the massive planets. paper   arxiv, VLT/NACO astrometry of the HR 8799 planetary system. HR 8799 Orbiting Exoplanets.gif 720 × 720; 980 KB. 2014 2009 paper, Pre-Discovery 2007 Image of the HR 8799 Planetary System Faster access than browser! paper, The Runts of the Litter: Why Planets Formed Through Gravitational Instability Can Only Be Failed Binary Stars & QUILLEN A. & JOHNSON J. 2013 paper   arxiv, Direct Detection and Orbit Analysis of the Exoplanets HR 8799 bcd from Archival 2005 Keck/NIRC2 Data Placing Limits on the Required Disk Masses 2018 MNRAS, 416, 1971 paper, Is the HR 8799 extrasolar system destined for planetary scattering? IV. Hence, there may be an unexplained misalignment between the rotation of the star and the orbits of its planets. CURRIE Th., BURROWS A., ITOH Y., MATSUMURA S., FUKAGAWA M., APAI D., MADHUSUDHAN N., HINZ Ph., RODIGAS T., KASPER M., PYO T.-S. & OGINO S. MNRAS, 419, 3074 & 5 additional authors D'ANGELO G., DURISEN R. & LISSAUER J. Nature, 468, 1080 [7] Near-infrared observations with the Project 1640 integral field spectrograph on the Palomar Observatory have shown that compositions between the four planets vary significantly. HR 8799 is a young (about 60 million years old) main-sequence star of spectral type A5 V located 128 light-years from Earth in the constellation Pegasus. paper   arxiv, Asteroseismic determination of the physical characteristics of the planetary system host HR 8799 (λ Bootis nature and age) 2011 Planetary systems with the best-fit masses from evolutionary models would be stable if the outer three planets are in a 1:2:4 orbital resonance (similar to the Laplace resonance between Jupiter's inner three Galilean satellites: Io, Europa and Ganymede as well as three of the planets in the Gliese 876 system). ApJ Letters, 794, L15 HR 8799: HR 8799A: IRAS 23050+2051: 2MASS J23072869+2108033: PPM 115157: SAO 91022: TD1 29627: TYC 1718-2350-1: uvby98 100218396: V* V342 Peg: WISE J230728.78+210802.8: Gaia DR2 2832463659640297472: Gaia DR1 2832463655344301952 & CARTER A. Astron. Science, 322, 1335 MAROIS C., MacINTOSH B., BARMAN T., ZUCKERMAN B., SONG I., PATIENCE J., LAFRENIERE D. & DOYON R. paper   arxiv, Estimation of the XUV radiation onto close planets and their evaporation 2018 CURRIE Th., FUKAGAWA M., THALMANN Ch., MATSUMURA S. & PLAVCHAN P. Content paper, Atmospheric Characterization of Directly Imaged Exoplanets with JWST/MIRI J., 155, 226 The star's spectral type is therefore written as kA5 hF0 mA5 V; λ Boo. 2010 The dashed lines in the small insets connect the position of the planet at each epoch with the star. HELLED R. & BODENHEIMER P. 2013 ApJ, 755, 38 2009 ABSIL O. HINZ Ph., RODIGAS T., KENWORHY M., SIVANANDAM S., HEINZE A., MAMAJEK E. & MEYER M. & HAGHIGHIPOUR N. HR 8799 d is an exoplanet orbiting the star HR 8799, located about 118.8 light-years (36.4 pc) away from Solar System. It is 1.6 times more massive and 1.5 times bigger compared with our Sun. BOOTH M., JORDAN A., CASASSUS S., HALES A., DENT W. et al. ZURLO A., VIGAN A., GALICHER R., MAIRE A.-L., MESA D. et al. PATIENCE J., BULGER J., KING R., AYLIFFE B., BATE M. & 5 additional authors Warm dust (T ~ 150 K) orbiting within the innermost planet (e). paper, Metallicity of the Massive Protoplanets Around HR 8799 if Formed by Gravitational Instability paper   arxiv, Direct Imaging of Extra-solar Planets - Homogeneous Comparison of Detected Planets and Candidates Correlations with disk metallicity, mass and lifetime MADHUSUDHAN N., AGUNDEZ M., MOSES J. The HR 8799 system harbors four super-Jupiters orbiting with periods that range from decades to centuries. The positions of the star and the orbits of the four known planets are shown schematically. Zorerema's thick atmosphere render observation of its surface challenging in visible light, and the first detailed maps did not emerge until the arrival of the Magellan orbiter 22 years ago. & 44 additional authors paper  arxiv  ADS, Characterizing the Atmospheres of the HR8799 Planets with HST/WFC3 Statistically, for stars hosting a debris disk, the luminosity of this star suggests an age of about 20–150 million years. abstract, Imaging The Exoplanets In HR8799 With A Vector Vortex Coronagraph On The Palomar 1.5 M Diameter Well-corrected Subaperture G. Chauvin paper   arxiv, Observational Constraints on Companions inside of 10 AU in the HR 8799 Planetary System 2009 We also present a K-band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. 2009 According to dynamical simulations, the HR 8799 planetary system may be even an extrasolar system with multiple resonance 1:2:4:8. SKEMER A., MARLEY M., HINZ Ph., MORZINSKI K., STRUTSKIE M. & 13 additional authors BAAS, 41, no 2, 434.10 Astron. [33], This disk is so thick that it threatens the young system's stability.[34]. BAAS, 41, no 3, 31.03 arxiv   Astrobiol., 9, 259 arxiv, Imaged sub-stellar companions: not as eccentric as they appear? CREPP J. ApJ. paper   arxiv, Formation and evolution of planetary systems: the impact of high angular resolution optical techniques The inner edge of this belt is approximately in 3:2 resonance with said planet, similar to. & Astrophys., 459, A52 METCHEV S., MAROIS Ch. 2019 MATTHEWS B., KENNEDY G., SIBTHORPE B., BOOTH M., WATT M. & 3 additional athors FRANTSEVA K., MUELLER M., POKORNY P., van der TAK F. & ten KATE I. Rev., 18, 317 Further constraints on the planet architecture of the HR 8799 system & WILLIAMS J. paper  arxiv, Shaping HR8799’s outer dust belt with an unseen planet GOZDZIEWSKI K. & MIGASZEWSKI C. arxiv, HELIOS–RETRIEVAL: An Open-source, Nested Sampling Atmospheric Retrieval Code; Application to the HR 8799 Exoplanets and Inferred Constraints for Planet Formation 2015 paper  arxiv, Resolving the Planetesimal Belt of HR 8799 with ALMA 2018 & Astrophys., 532, A79 JGR Planets, accepted [27], Moderate-resolution near-infrared spectroscopy, obtained with the Keck telescope, definitively detected carbon monoxide and water absorption lines in the atmosphere of planet c. The carbon-to-oxygen ratio, which is thought to be a good indicator of the formation history for giant planets, for planet c was measured to be slightly greater than that of the host star HR 8799. INGRAHAM P., MARLEY M., SAUMON D., MAROIS Ch., MACINTOSH B. et al. 2011 MNRAS arxiv   2009 2011 ApJ., 729, 128 2011 SCHNEIDER J., DEDIEU C., LE SIDANER P., SAVALLE R. & ZOLOTUKHIN I. paper, Homogeneous comparison of planet candidates imaged directly until 2008 arxiv, Space Technology for Directly Imaging and Characterizing Exo-Earths arxiv, First light of the VLT planet finder SPHERE. KONOPACKY Q., MACINTOSH B., MAROIS C., BARMAN T. & GHEZ A. This image shows three planets orbiting the star HR 8799. Sci. & WYATT M. arxiv  paper   arxiv, Exoplanet Atmospheres MNRAS, 406, 566 2017 GOZDZIEAWSKI K. & MAGASZEWSKI C. Dit is deel van ’n stelsel wat ook ’n rommelskyf en minstens vier gasreuse bevat. 2016 2010 Its discovery was publicly announced on 2008. 2009 LAVIE, B., MENDOÇA, J., MORDASINI, C. & 7 additional authors BAAS, 42, no 1, 377.07 444226main exoplanet20100414-a-full.jpg 1,024 × 768; 47 KB. 2012 & HU Y. 2018 2018 paper  arxiv   SKEMER A., HINZ Ph., ESPOSITO E., BURROWS A., LEISENRING J. 2009 2009 Captured in 2008 using Keck Observatory’s near-infrared adaptive optics, the picture revealed three planets (labeled ‘b’, ‘c’, and ‘d’) orbiting a dusty young star named HR 8799 (center). III. The spectrum, with a signal-to-noise ratio of $\approx 5$ per spectral channel, is compatible with a late-type L brown dwarf. Astron. paper  arxiv, First Light LBT AO Images of HR 8799 bcde at 1.65 and 3.3 Microns: New Discrepancies between Young Planets and Old Brown Dwarfs HR 8799 is a 30 million-year-old star located approximately 129 light-years away from Earth in the constellation Pegasus.. paper   arxiv   ADS, Clouds and Chemistry in the Atmosphere of Extrasolar Planet HR8799b paper, Thermal Infrared MMTAO Observations of the HR 8799 Planetary System WANG J., GRAHAM J., DAWSON R., FABRYCKY D., DE ROSA R. et al. 2011 Bintang i ni memiliki sekitar 1,5 kali massa Matahari dan 4,9 kali luminositas matahari. The planet orbits at 24 AU from HR 8799 with an eccentricity greater than 0.04 and a period of 100 years. Download Unionpedia on your Android™ device! paper  arxiv  ADS, The dynamical structure of HR 8799's inner debris disk 2013 abstract, The Formation Mechanism of Gas Giants on Wide Orbits READ M., WYATT M., MARINO S. & KENNEDY G. paper, M-band Imaging of the HR 8799 Planetary System Using an Innovative LOCI-based Background Subtraction Technique 2009 GALICHER, R., MAROIS, C., MACINTOSH, B., ZUCKERMAN, B., BARMAN, T. & 6 additional authors & Astrophys., in press 2009 ApJ., 753, 14 The luminosity profile of the Balmer lines in the star's spectrum, as well as the star's effective temperature, best match the typical properties of an F0 V star. ApJS, accepted 2020 abstract, Direct Imaging of Multiple Planets Orbiting the Star HR 8799   MOYA A., AMADO J., BARRADO D., GARCIA HERNANDEZ A., ABERASURI M., MONTESINOS B. Credit: C. Marois et al., NRC Canada. 2016 Astron. L0-band observations of the three outer planets GOZDZIEWSKI K. & MIGASZEWSKI C. 2011 BARUTEAU C., MERU F., PAARDEKOOPER S.-J. & GILLON M. 2010 arxiv, First light of the VLT planet finder SPHERE. & Astrophys., 531, L17 & Astrophys. The star is a Gamma Doradus variable: its luminosity changes because of non-radial pulsations of its surface. preprint, The Debris Disk Around HR 8799 A dramatic halo of small grains originating in the cold dust component. Astron. MADHUSUDHAN N., BURROWS A. SUDOL J. The best accepted value for an age of HR 8799 is 30 million years, consistent with being a member of the Columba association co-moving group of stars. 2009 SANZ-FORCADA J., MICELA G., RIBAS I., POLLOCK A., EIROA C. & 2 additional authors 2012 & ACEITUNO F. GALICHER R., MAROIS Ch., MACINTOSH B., BARMAN T. & KONOPACKY Q. HR 8799 is a roughly 30 million-year-old main-sequence star located 129 light-years (39.6 parsecs) away from Earth in the constellation of Pegasus. Exoplanet Comparison HR 8799 d.png 1,040 × 480; 171 KB. [12] Observation of this star with the Chandra X-ray Observatory indicates that it has a weak level of magnetic activity, but the X-ray activity is much higher than that of an A-type star like Altair. 4.9 Bintang i ni adalah bagian dari sistem yang juga berisi disk puing dan setidaknya empat planet besar. Letters, 730, L21 paper   arxiv, Dynamical evolution of planetary systems All three companions are confirmed as co-moving with HR 8799 to 98 σ for b, 90 σ for c and ∼6 σ for d. Counter-clockwise orbital motion is observed for all three companions. BAAS, 42, no 1, 377.06 HR 8799 HR 8799 je přibližně 30 milionů let stará hvězda hlavní posloupnosti v souhvězdí Pegase, vzdálená 129 světelných roků (39,6 parseků) od Země. paper   Science   astro-ph, Seeing is Believing Rev. 2010 2016 2017 ADS, The International Deep Planet Survey II: The frequency of directly imaged giant exoplanets with stellar mass ApJ, 795, 133 & Astrophys., 47, 253 ADS, Thermal Infrared Imaging and Atmospheric Modeling of VHS J125601.92-125723.9 b: Evidence for Moderately Thick Clouds and Equilibrium Carbon Chemistry in a Hierarchical Triple System The host star HR 8799 has apparent magnitude of 6.0, with absolute magnitude of 3.2. arxiv  MATTHEWS, E., HINKLEY, S., VIGAN, A., KENNEDY, G., SUTLIEFF, B. et al. ApJ. [36], Starting in 2010, astronomers searched for radio emissions from the exoplanets orbiting HR 8799 using the radio telescope at Arecibo Observatory. MORBIDELLI A. HINKLEY S. ApJ. MAROIS Ch., MACINTOSH B., BARMAN T., ZUCKERMAN B., SONG I., PATIENCE J., LAFRENIERE D. & DOYON R. paper   2011 REIDMEISTER M., KRIKOV A., SCHMIDT T., FIEDLER S., MÜLLER S., LÖHNE T. & NEUHÄUSER R. 2016 ApJ, accepted It is part of a system that also contains a debris disk and at least four massive planets. arxiv, Multiple mean motion resonances in the HR 8799 planetary system New constraints on the HR 8799 planetary system from mid-infrared direct imaging 2019 PETIT dit de la ROCHE D., van den ANKER M., KISSLER-PATIG M., IVANOV V. & FEDELE D. MNRAS, 491, 1795 ApJ., 737, Issue 1, 34, 15 pp & IRELAND M. DEMING D. & SEAGER S. Astrophys., 48, 631 The inner and outer edges of this belt are close to 4:1 and 2:1 resonances with the planet. The near-infrared spectra from this instrument confirmed the red colors of all four planets and are best matched by models of planetary atmospheres that include clouds. 2016 Nature Astron., 2, 600 The star is also poor in elements heavier than sodium: for example, the iron abundance is only 28% of the solar iron abundance. paper  arxiv  ADS, Astrometric Monitoring of the HR 8799 Planets: Orbit Constraints from Self-Consistent Measurements ADS, The Habitable Exoplanet Observatory & Astrophys., 594, A64 paper, H band Image of a Planetary Companion around HR 8799 in 2002 ApJ, 823, 149 NIELSEN E., DE ROSA R., MACINTOSH B., WANG J., RUFFIO J.-B. Astron. ApJ., 710, 1408 paper  arxiv, Performance and Early Science with the Subaru Coronagraphic Extreme Adaptive Optics Project BAAS, 4, 302.04 BOSS A. Astron J, 154, 91 ApJ, 830, 114 ApJ., 754, 135 Planeettojen nimet ovat etäisyysjärjestyksessä HR 8799 d, HR 8799 c ja HR 8799 b. Planeettojen massat ovat noin 5-13 Jupiterin massaa. 2017 2011 2016 2016 ApJ., 733, 126 J. BAAS, 41, no 3, 05.06 CURRIE Th. 2017 HR 8799 adalah bintang urutan utama berusia 30 juta tahun terletak 129 tahun cahaya (39,6 parsec) dari Bumi di konstelasi Pegasus. 2018

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