the Solar eclipse of August 11, 1999 total eclipse of 1999 The chromosphere literally, sphere of colour ... of the chromosphere is very small, it being only math 10 4 math times that of the photosphere , the layer just below it, and math 10 8 math times that of the atmosphere of Earth . This makes the chromosphere ... 762 isbn 978 0716785842 ref However, without special equipment, the chromosphere cannot normally be seen due to the overwhelming brightness of the photosphere. Although relatively thin, the density of the chromosphere ... and density vary with height. Comparing chromosphere and photosphere Whilst the photosphere has an Spectral lines Types of line spectra absorption line spectrum, the chromosphere s spectrum is dominated ... causes the chromosphere to have its characteristic reddish colour. By analysing the spectrum of the chromosphere ... with increasing height in the chromosphere itself. Its temperature at the top of photosphere is only about math 4400 math K, whilst at the top of chromosphere, some math 2,000 math km higher, it reaches ... of the of the chromosphere to paradoxically increase as you move away from the Sun s interior ... to the prediction of space weather . Solar prominence s rise up through the chromosphere from ... below. Spicules rise to the top of the chromosphere and then sink back down again over the course ... chromosphere Eclipse of March 7, 1970 . See also Plage astronomy Orders of magnitude density ... Animated explanation of the Chromosphere and Transition Region University of Glamorgan . http ... of the Chromosphere and Transition Region University of Glamorgan . The Sun Star Category Sun ar ... more details
Wiktionarypar plage Plage may refer to Plage astronomy , a bright region in the chromosphere of the Sun Plage mycology , a clear, unornamented area on the basal area of an ornamented fungal spore disambig er fr Plage homonymie io Plajo homonimo ja ... more details
Image Mauna Loa Solar Observatory.jpg thumb 270px Two domes house the sensors The Mauna Loa Solar Observatory MLSO is a collection of instruments for observing Sun the sun located on the slopes of the Mauna Loa volcano on the Hawaii island island of Hawaii , USA at an elevation of convert 11135 ft m . General information The MLSO is operated by the High Altitude Observatory , which is a laboratory within the National Center for Atmospheric Research . The observatory is tasked with monitoring the Sun solar Stellar atmosphere atmosphere and recording data on Plasma physics plasmic and energy energetic emissions from the chromosphere and corona . Studies of Coronal Mass Ejection s CMEs are conducted at MLSO. All data are available from the MLSO web page http mlso.hao.ucar.edu ref cite web url http mlso.hao.ucar.edu title Mauna Loa Solar Observatory publisher official web site accessdate 2009 07 04 ref Instruments The MLSO contains instruments to record images of the solar disc and limb, every 3 minutes between 17 00 UT and 0230 UT weather permitting. The instruments currently operated at the observatory are MK4 K Coronameter White Light Corona field of view 1.09 to 2.79 solar radii PICS Ha Limb Disk Chromosphere 1600 km Decommissioned Coronado Solarmax 60 Ha Limb Disk Imagining Chromosphere CoMP Coronal Multi channel Polarimeter Near IR Coronal Polarimeter CHIP Helium I Imager Chromosphere 2000 km and coronal holes PSPT Photosphere surface and the chromosphere 400 km The site is shared with the Mauna Loa Observatory run by the National Oceanographic and Atmospheric Administration at coordinates coord 19 32 10 N 155 34 34 W type landmark region US HI display inline,title , about two miles north of Mokuaweoweo , the summit of Mauna Loa. References reflist Category Astronomical observatories in Hawaii Category Buildings and structures in Hawaii County, Hawaii astronomy stub Hawaii stub zh ... more details
Summary A cartoon depicting the different scales of coronal loop that exist in the lower corona and transion region . Many scales have been observed and it is believed there are many sub Sensor resolution resolution structures below the transition region threading through the chromosphere . Highly radiating coronal loops may share the same footpoint location as open flux tubes i.e. solar wind and coronal holes and therefore may share similar physics leading to the conjecture that coronal loops may share similar heating mechanisms as the solar wind. Cartoon produced by http www.astroengine.net Dr Ian O Neill and can be found in the thesis entitled http www.astroengine.net astro alfvenwave thesis06.pdf Quiescent Coronal Loops Heated by Turbulence . Licensing PD self date January 2007 Orphan image Copy to Wikimedia Commons bot Fbot ... more details
Summary Public domain This file is in the public domain because it was created by NASA. NASA copyright policy states that NASA material is not protected by copyright unless noted . NASA copyright policy page or JPL Image Use Policy . Original Caption Release with Image Extreme Ultraviolet Imaging Telescope EIT image of a huge, handle shaped prominence taken on Sept. 14,1999 taken in the 304 angstrom wavelength Prominences are huge clouds of relatively cool dense plasma suspended in the Sun s hot, thin corona. At times, they can erupt, escaping the Sun s atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K. Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. Source http photojournal.jpl.nasa.gov catalog ?IDNumber PIA03149 Licensing PD USGov NASA Copy to Wikimedia Commons bot Svenbot ... more details
Unreferenced date December 2009 For the genus of gossamer winged butterflies , see Facula butterfly . Image Sun at 304 Angstroms.jpg thumb right 256px The bright areas visible here on the Sun are faculae . A facula plural faculae , Latin for little torch , is literally a bright spot. It is used in planetary nomenclature for naming certain surface features of planets and moons, and is also a type of surface phenomenon on the Sun . Solar faculae are bright spots that form in the canyons between Granule solar physics solar granules , short lived convection cells several thousand kilometers across that constantly form and dissipate over timescales of several minutes. Faculae are produced by concentrations of magnetic field lines. The Sun The chromosphere is above the photosphere. Solar energy passes through this region on its way out from the center of the Sun. Faculae and flares arise in the chromosphere. Faculae are bright luminous hydrogen clouds which form above regions where sunspots are about to form. Flares are bright filaments of hot gas emerging from sunspot regions. Sunspots are dark depressions on the photosphere with a typical temperature of 4,000 C 7,000 F . source http www.solarviews.com eng sun.htm Category Stellar phenomena Category Solar phenomena ar ca F cula de Sonnenfackel es F cula eo Suntor o fr Facula hr Fakula ko it Facula he hu Napfolt ml nl Zonnevlek ja pl Flokule pt Manchas solares ru sk Fakula sl Son eva pega fi Auringonpilkku sv Solfl ckar th zh ... more details
A plage is a bright region in the chromosphere of the Sun , typically found in regions of the chromosphere near sunspots . The term itself is poetically taken from the French word for beach. The plage regions map closely to the faculae in the photosphere below, but the latter have much smaller spatial scales. Accordingly plage occurs most visibly near a sunspot region. Faculae have a strong influence on the solar constant , and the more readily detectable because chromospheric plage areas traditionally are used to monitor this influence. In this context active network consists of plage like brightenings extending away from active regions as their magnetism appears to diffuse into the quiet Sun, but constrained to follow the network boundaries. Because we can explain faculae with the strictly photospheric hot wall model, ref cite journal doi 10.1086 304295 last Topka first K. P. coauthors Tarbell, T. D. Title, A. M. year 1997 title Properties of the Smallest Solar Magnetic Elements. II. Observations versus Hot Wall Models of Faculae journal Astrophysical Journal volume 484 issue 1 pages 479 486 bibcode 1997ApJ...484..479T ref it is not clear what the actual physical relationship between plage and faculae may be. References reflist External links http www.daviddarling.info encyclopedia P plage.html Encyclopedia of Astrobiology, Astronomy & Spaceflight Plage the Sun Category Stellar astronomy Category Stellar phenomena Category Sun Category Solar phenomena sun stub ca Platja astronomia lt Flokulas ro Plaj solar sk Flokula zh ... more details
saved book title subtitle cover image cover color The Sun Overview Sun Internal Structure Standard solar model Solar core Radiation zone Convection zone Atmosphere Stellar atmosphere Photosphere Photosphere Supergranulation Granule solar physics Granule Facula Sunspot Sp rer s law Joy s Law astronomy Joy s Law Chromosphere Chromosphere Plage astronomy Plage Spicule solar physics Spicule Moreton wave Corona Corona Solar transition region Coronal hole Coronal loop Coronal mass ejection Coronal radiative losses Solar prominence Helmet streamer Nanoflares Variation Solar variation Solar cycle List of solar cycles Solar maximum Solar minimum Wolf number Solar flare Helioseismology 160 minute solar cycle Solar neutrino problem Solar rotation Differential rotation Carrington rotation Tachocline Sp rer Minimum Maunder Minimum Dalton Minimum Modern Maximum Heliosphere Heliosphere Solar wind Heliospheric current sheet Bow shock Faint young Sun paradox Solar probe missions Pioneer 5 Pioneer 6, 7, 8, and 9 Helios spacecraft Helios International Cometary Explorer Ulysses spacecraft Ulysses WIND spacecraft WIND Solar and Heliospheric Observatory Solar and Heliospheric Observatory SOHO Advanced Composition Explorer Genesis spacecraft Genesis STEREO Proposed missions Solar Sentinels Solar Probe Plus Solar Orbiter Category Wikipedia books on astronomy The Sun ... more details
of the sun we see shining every day, the photosphere. ref Observed during eclipse, the sun s chromosphere ... the chromosphere of giant stars visible. ref Cite book last1 Griffin first1 R.E. editor1 first W.I. ... SEE a Stellar Chromosphere url http journals.cambridge.org action displayAbstract jsessionid ... more details
Infobox observatory name Kanzelhoehe Solar Observatory image caption organization University of Graz Karl Franzens University code location Villach , Austria coords coord 46 40.7 0 N 13 54.4 0 E type landmark region AT altitude 1,526 meters 5,006 feet weather established Start date YYYY MM DD closed website URL http www.solobskh.ac.at The Kanzelhoehe Solar Observatory or KSO is an astronomy astronomical observatory affiliated with the Institute of Geophysics, Astrophysics and Meteorology out of the University of Graz Karl Franzens University . It is located near Villach on the southern border of Austria . Its Web page at http www.solobskh.ac.at usually posts current images of the sun, especially in the hydrogen alpha line that is the strongest visible light line of hydrogen and that reveals the solar chromosphere. History Founded in 1943 by the German Luftwaffe to research the effects of the Sun on the Earth s ionosphere , the KSO focuses on multispectral synoptic observations of the sun using several telescope on the same mount. External links http www.solobskh.ac.at www.solobskh.ac.at observatory stub Category Astronomical observatories in Austria de Sonnenobservatorium Kanzelh he ... more details
Lyman continuum . This condition holds at the top of the chromosphere , where the equilibrium temperature ... sunStructure.html transitionregion Animated explanation of the Transition Region and Chromosphere ... Animated explanation of the temperature of the Transition Region and Chromosphere University of Glamorgan ... more details
Infobox Album See Wikipedia WikiProject Albums Name Microgravity Type Album Artist Biosphere musician Biosphere Cover Biosphere Microgravity.JPG Released 1992 Recorded ? Genre Ambient house Length 47 11 Label Apollo Records Belgium Apollo Producer Biosphere musician Geir Jenssen Last album This album Microgravity br 1992 Next album Patashnik br 1994 Album ratings rev1 Allmusic rev1Score Rating 5 5 ref Allmusic class album id r170487 pure url yes ref Microgravity is the debut album by Biosphere musician Biosphere , released in 1992. Track listing Microgravity 5 12 Baby Satellite 5 04 Tranquillizer 8 18 The Fairy Tale 4 53 Cloudwalker II 5 26 Chromosphere 3 28 Cygnus A 5 02 Baby Interphase 5 07 Biosphere 4 41 Personnel Biosphere musician Geir Jenssen Alexander Stojanovic References reflist Biosphere Category 1992 albums Category Biosphere albums Category Debut albums 1990s electronic album stub ... more details
cleanup date November 2010 refimprove date November 2010 The Solar Dynamics Observatory SDO Atmospheric Imaging Assembly AIA , led from the Lockheed Martin Solar and Astrophysics Laboratory LMSAL , provides full disk imaging of the Sun in several ultraviolet and extreme ultraviolet EUV band passes at high spatial and temporal resolution. The four telescopes that provided the individual light feeds for the instrument were designed and built at the Smithsonian Astrophysical Observatory SAO . class wikitable AIA Wavelength Channel Region of solar atmosphere Characteristic br Temperature White Light Photosphere 5000 K 1700 Temperature minimum, photosphere 5000 K 1600 Transition region & photosphere 10 5 & 5000 K 304 Chromosphere & transition region 50,000 K 171 Quiet corona , upper transition region 6.3x10 5 K 193 Corona & hot Solar flare flare Plasma physics plasma 1.2x10 6 & 2x10 7 K 211 Active region corona 2x10 6 K 335 Active region corona 2.5x10 6 K 94 Solar flare Flaring regions 6.3x10 6 K 131 Solar flare Flaring regions 4x10 5, 10 7 & 1.6x10 7 K Category Sun ... more details
Image Spicules sst big.jpg thumb Spicules, visible as dark tubes. Solar active region 10380, June 2004 In solar physics , a spicule is a dynamic jet of about 500 km diameter in the chromosphere of the Sun . It moves upwards at about 20 km s from the photosphere . They were discovered in 1877 by Father Angelo Secchi of the Vatican Observatory in Rome. Description Spicules last for about 15 minutes ref name Freedman cite book last1 Freedman first1 Roger A. last2 Kaufmann III first2 William J. title Universe publisher W. H. Freeman and Company date 2008 location New York, USA pages 762 isbn 978 0716785842 ref at the solar limb they appear elongated if seen on the disk, they are known as mottles or fibrils . They are usually associated with regions of high magnetic flux their mass flux is about 100 times that of the solar wind . They rise at a rate of math 20 math km s or math 72,000 math km h and can reach several thousand kilometers in height before collapsing and fading away. Prevalence There are about 300,000 active spicules at any one time on the Sun s chromosphere , amounting to about 1 of the Sun s surface ref name Freedman .At any one time there are around 60,000 to 70,000 active spicules on the Sun an individual spicule typically reaches 3,000 10,000 km altitude above the photosphere. ref § 1, Two Dynamical Models for Solar Spicules, Paul Lorrain and Serge Koutchmy, Solar Physics 165 , 1 April 1996 , pp. 115 137, doi 10.1007 BF00149093 , bibcode 1996SoPh..165..115L . ref Causes Bart De Pontieu Lockheed Martin Solar and Astrophysics Laboratory , Palo Alto, California , Robert Erd lyi and Stewart James both from the University of Sheffield , Sheffield, UK hypothesised in 2004 that spicules formed as a result of Helioseismology P mode oscillations in the Sun s surface, sound waves with a period of about five minutes that causes the Sun s surface to rise and fall at several hundred meters per second see helioseismology . Magnetic flux tubes that ... more details
, Chromosphere etc. or inspired by the wisdom, culture and artefacts of the ancient and medieval ... of Stars Desert Dances Elektron Musik available from his web site as a burn to order cd Chromosphere ... more details
in physics from Yeshiva University in 1969 his thesis was on The Heating of the Solar Chromosphere ... Chromosphere author Gruber, Gary Richard date 1969 work publisher accessdate May 1, 2011 ref He lives ... more details
Olin Chaddock Wilson January 13, 1909 &ndash July 13, 1994 was an American astronomer best known for his work as a stellar spectroscopy spectroscopist . Born in San Francisco, CA as the son of a lawyer , Wilson showed an interest in physics at an early age. He studied astronomy and physics at the University of California, Berkeley and wrote his first scientific paper in 1932 on the subject of the speed of light . He received his Doctor of Philosophy PhD from the California Institute of Technology in 1934. Wilson was a staff member of Mount Wilson Observatory not named after Olin Wilson for most of his research career where he studied star stellar chromosphere s. He was the first scientist to discover activity cycles, similar to the sun solar 11 year sunspot cycle, in other stars. In collaboration with Vainu Bappu , an Indian astronomer, he also showed that there was a correlation between the width of the Ca II lines in stellar spectrum spectra and the star s luminosity , the Wilson Bappu Effect . He gave the Henry Norris Russell Lectureship in 1977 and won the Bruce Medal in 1984.. External links http www.nap.edu readingroom books biomems owilson.html National Academy of Sciences biography Persondata Metadata see Wikipedia Persondata . NAME Wilson, Olin ALTERNATIVE NAMES SHORT DESCRIPTION DATE OF BIRTH January 13, 1909 PLACE OF BIRTH DATE OF DEATH July 13, 1994 PLACE OF DEATH DEFAULTSORT Wilson, Olin Category 1909 births Category 1994 deaths Category American astronomers US astronomer stub de Olin C. Wilson fr Olin Wilson it Olin Chaddock Wilson lb Olin C. Wilson nl Olin Wilson sl Olin Chaddock Wilson ... more details
BY Draconis variables are main sequence variable star s of stellar classification late spectral types , usually K or M. The name comes from the archetype for this category of variable star system, BY Draconis . They exhibit variations in their luminosity due to rotation of the star coupled with star spot s, and other chromosphere chromospheric activity. ref name MLM cite journal author Lopez Morales, Mercedes Morrell, N. I. Butler, R. P. Seager, S. title Limits to Transits of the Neptune mass planet orbiting Gl 581 journal Publications of the Astronomical Society of the Pacific year 2006 volume 118 pages arxiv astro ph 0609255 quote BY Draconis variable. This type of variable is characterized by quasiperiodic photometric variations over time scales from less than a day to months, and amplitudes ranging from a few hundredths of a magnitude to 0.5 mags. bibcode 2006PASP..118.1506L doi 10.1086 508904 ref Resultant brightness fluctuations are generally less than 0.5 Apparent magnitude magnitudes ref name MLM on timescales equivalent to the star s rotational period, typically from a fraction of a day to several months. Some of these stars may also have flares, resulting in additional variations of the UV Ceti variable UV Ceti type . Oddly enough, Procyon the 8th brightest night time star which is an F5 sub giant or dwarf has also been classified as a BY Draconis variable. Source Schaaf, The Brightest Stars , Wiley, 2008. References reflist Samus N.N., Durlevich O.V., et al. Combined General Catalog of Variable Stars GCVS4.2, 2004 Ed. Schaaf, Fred, The Brightest Stars , Wiley, 2008 Variable star topics DEFAULTSORT By Draconis Variable Category BY Draconis variables Category Variable stars var star stub ca Variable BY Draconis de BY Draconis Stern es Estrella variable BY Draconis fr Variable de type BY Draconis it Variabile BY Draconis ja BY ru BY fi BY Draconis muuttuja tr BY Draconis de i eni zh BY ... more details
The Interface Region Imaging Spectrograph or IRIS is a planned space probe to observe the Sun by NASA . It is a NASA Small Explorer program mission to investigate the physical conditions of the solar limb, particularly the chromosphere of the Sun . It will be built and operated by the Lockheed Martin Solar and Astrophysics Laboratory, and launched in late 2012 by a Pegasus rocket . Its instrument is a high frame rate UV imaging spectrometer one image a second, 0.3 arcsec spatial resolution, and sub angstrom spectral resolution. NASA announced on June 19, 2009 that the IRIS was selected from six small explorer mission candidates ref cite web url http www.nasa.gov home hqnews 2008 may HQ C08029 SMEX Awards.html title NASA Selects Small Explorer Investigations for Concept Studies publisher NASA ref , along with Gravity and Extreme Magnetism SMEX . ref cite web url http www.nasa.gov home hqnews 2009 jun HQ 09 141 SMEX Selections.html title NASA Awards Two Small Explorer Development Contracts publisher NASA date 2009 06 19 ref IRIS team Science and engineering team members include ref http iris.lmsal.com ref Lockheed Martin Solar and Astrophysics Lab Lockheed Martin Sensing and Exploration Systems Smithsonian Astrophysical Observatory Montana State University Bozeman Institute for Theoretical Astrophysics, University of Oslo High Altitude Observatory, NCAR Stanford University NASA Ames Research Center NASA Goddard Space Flight Center National Solar Observatory Space Sciences Lab, UC Berkeley Princeton Plasma Physics Laboratory Sydney Institute for Astronomy, University of Sydney Center for Plasma Astrophysics, University of Leuven Mullard Space Science Laboratory Rutherford Appleton Laboratory European Space Agency Max Planck Institut fuer Sonnensystemforschung National Astronomical Observatory, Tokyo Niels Bohr Institute , University of Copenhagen References reflist External links http iris.lmsal.com Interface Region Imaging Spectrograph Category Proposed spacecraft Cat ... more details
. ref cite journal last Withbroe, G.L., Noyes, R.W. title Mass and energy flow in the solar chromosphere ... towards the chromosphere along the arcs. In the transition region where the temperature is about 10 ... how this energy is transmitted from the chromosphere where it could be absorbed or reflected , and then dissipated ... can go through the chromosphere and transition region , carrying an energy flux comparable to that required to sustain the corona . Anyway wave train periods observed in the high chromosphere ... cloud ColBreak Photosphere Chromosphere Transition region Stellar active region ColBreak Magnetic reconnection ... more details
expert subject date March 2011 File KW326Kprof.jpg thumb K line spectrum of KW 326, a dwarf star in the Praesepe open cluster. The line is very wide and very deep, and it originates in the photosphere, just like any other absorption line. Several other lines are superimposed on it. In the center, the emission due to the K line itself, which takes place in the chromosphere. Image Kcore.jpg thumb Zoom on the emission core. W0 is defined as the difference in wavelength between the points on either side of the emission at an average intensity between the K1 minimum and the K2 maximum The Ca II K line in cool stars is among the strongest absorption line s. A small emission electromagnetic radiation emission , which originates in the chromosphere , is present in its core. In 1957, Olin Chaddock Wilson Olin C. Wilson and Manali Kallat Vainu Bappu M. K. Vainu Bappu reported on the remarkable correlation between the measured width of the aforementioned emission line and the Absolute Magnitude absolute visual magnitude of the star . ref http ads.nao.ac.jp abs 1957ApJ...125..661W, Wilson O.C. Bappu, V. 1957 H and K Emission in Late Type Stars Dependence of Line Width on Luminosity and Related Topics. Astrophysical Journal, vol. 125, p.661 ref This is known as the Wilson Bappu effect . The correlation is independent of spectral type and applicable to stellar classification stars of type G type main sequence star G , K type main sequence star K , and Red giant M . The wider the absorption, the brighter the star. The main interest of the Wilson Bappu effect resides in its potential as a distance indicator, which is a consequence of the following facts the Wilson Bappu effect can be studied using nearby stars, for which independent distance measurements are possible, and it can be expressed in a simple analytical form, in other words, the Wilson Bappu effect can be calibrated with stars within 100 pc from the Sun the width of the emission core of the K line W0 can be measured in d ... more details
and IM Pegasi http adsabs.harvard.edu full 1989ApJ...339.1059B The active chromosphere binary HD 17433 ... active stars http adsabs.harvard.edu full 1988ApJS...68..803B H alpha spectroscopy of active chromosphere ... more details
Starbox short name HD 81040 epoch J2000 constell Leo constellation Leo ra 09 sup h sup 23 sup m sup 47.0873 sup s sup dec 20 21 52.034 appmag v 7.74 dist ly 106.2 dist pc 32.56 spectral G2 G3 names BD 20 2374, FK5 4836, GC 12951, HIP 46070, SAO 80800 Simbad HD 81040 HD 81040 is a star in the constellation of Leo constellation Leo . It is G type yellow dwarf like our Sun . The Sun dwarfs HD 81040 in terms of physical characteristics. The age of the star is not precisely known the ELODIE spectrograph suggested 0.8 Gyr and found it to have a young dust disk. Later measurements by modelling chromosphere chromosperic activity suggested an age of 4.18 Gyr. Planetary system On November 24, 2005, a superjovian planet was announced by Sozzetti. OrbitboxPlanet begin table ref ref cite journal url http www.aanda.org articles aa abs 2006 13 aa4303 05 aa4303 05.html author Sozzetti et al. title A massive planet to the young disc star HD 81040 journal Astronomy and Astrophysics volume 449 issue 1 year 2006 pages 417 424 format abstract doi 10.1051 0004 6361 20054303 last2 Udry first2 S. last3 Zucker first3 S. last4 Torres first4 G. last5 Beuzit first5 J. L. last6 Latham first6 D. W. last7 Mayor first7 M. last8 Mazeh first8 T. last9 Naef first9 D. bibcode 2006A&A...449..417S arxiv astro ph 0511679 http arxiv.org abs astro ph 0511679 web preprint ref OrbitboxPlanet exoplanet HD 81040 b b mass 6.86 0.71 period 1001.7 7.0 semimajor 1.94 eccentricity 0.526 0.042 Orbitbox end See also List of extrasolar planets References reflist External links http exoplanet.eu star.php?st HD 81040 The Extrasolar Planets Encyclopaedia HD 81040 Sky 09 23 47.0873 20 21 52.034 106.2 Category G type main sequence stars Category Henry Draper Catalogue objects 81040 Category HIP objects 46070 Category Leo constellation main star stub Category Planetary systems de HD 81040 es HD 81040 fa fi HD 81040 ... more details
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