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Topic: Zeta Aurigae


  
  Auriga (constellation) - Wikipedia, the free encyclopedia
Auriga (Latin for charioteer) is a northern constellation.
Stars Alpha Aurigae, Beta Aurigae, Theta Aurigae, Iota Aurigae, and Eta Aurigae form the charioteer's head: with Alpha Aurigae being of magnitude zero, Beta Aurigae being of magnitude two, and the rest of the stars being of magnitude three.
Star Alpha Aurigae may be taken to represent the charioteer's eye, whereas star Iota Aurigae represents the charioteer's chin.
en.wikipedia.org /wiki/Auriga_(constellation)   (719 words)

  
 The Masses and Radii of the Eclipsing Binary zeta Aurigae
The zeta Aur K star primary presents no difficulty, and accurate radial velocities are readily obtainable in the optical.
The positions of the zeta Aur stars on the theoretical HR diagram are compared to current evolutionary model tracks, and the resulting good agreement provides a strong check of the internal self­consistency of this analysis and the accuracy of the theoretical models.
The zeta Aurigae stars are confirmed to be coeval witll an age of 80 ± 15 Myr.
casa.colorado.edu /Publications/preprints/1996/janapr/268.shtml   (372 words)

  
 Auriga Constellation   (Site not responding. Last check: 2007-10-11)
Auriga is an ancient Northern Hemisphere constellation featuring one of the brightest stars in the heavens: Capella.Auriga is usually pictured as a charioteer; the youth Auriga wields a whip in one hand and holds a goat
Auriga is usually pictured as a charioteer; the youth Auriga wields a whip in one hand and holds a goat (Capella) and her two kids in the other.
Zeta Aurigae is an eclipsing binary; an orange giant primary with a blue companion that orbits every 972 days (2.7 years).
www.udy.com /hosts/Wingmakers/Auriga.html   (1329 words)

  
 Zeta Aurigae
It is also known as Haedus I and by an astonishing coincidence, its constellation mate, Epsilon Aurigae, which is the second Kid ("Haedus II"), is also a well-known (and even more remarkable) eclipsing binary.
Zeta consists an orange supergiant (spectral type K4) in orbit around a blue B star (type B5) with a period of 972.2 days (2.66 years).
Because the orientation of the orbit lies within 3° of our line of sight, every 2.66 years the smaller B star hides completely behind the larger K star (which is about as wide as Venus's orbit), and the combined visual light drops by 0.15 magnitude (about 15%).
www.daviddarling.info /encyclopedia/Z/Zeta_Aurigae.html   (272 words)

  
 Auriga the Charioteer   (Site not responding. Last check: 2007-10-11)
Auriga depicts a Charioteer, who is crouched down and holding a nanny goat and her three kids.
Auriga's brightest star is Capella, the 6th brightest night time star at magnitude 0.08.
It and the stars Mu Columbae (in Columba the dove) and 53 Arietis (in Aries the ram) seem to be fleeing the star forming region in the constellation of Orion.
ourworld.compuserve.com /homepages/bmoler/auriga.htm   (636 words)

  
 Auriga   (Site not responding. Last check: 2007-10-11)
The name of the brightest star of the constellation, Capella, means a small goat, and the kids are the stars Epsilon, Eta, and Zeta Aurigae.
Alpha Aurigae - Capella is the northernmost star in the "winter hexagon" (0.1 mag, distance 42 light-years).
Epsilon Aurigae - Almaaz is a system of five stars, two of which form a remarkable eclipsing binary, the brightness of which drops from 2.9 snag to 3.8 mag once every 27 years.
www.avastronomyclub.org /const/aur.htm   (392 words)

  
 Auriga   (Site not responding. Last check: 2007-10-11)
Placed to the north of Gemini and Taurus, and situated between Lynx and Perseus, the constellation of Auriga contains the sixth star in order of brightness of the whole vault of heaven: it is Capella, a yellow giant, with a bright issue equal to sixty times that of the Sun.
Other interesting stars are two eclipse binaries, both situated near the border with the constellation of Perseus: epsilon Aurigae, that has a 27-year period (the longest among the known eclipse binaries), and zeta Aurigae, which every 2 years and 6 months pass during six weeks from the magnitude 3,7 to the magnitude 4,0.
Auriga, then, has a trio of open cluster: M36 (reproduced here on the left), that counts about sixty stars; M37, composed from around 150 stars; and M38, the least compact one, with hundred weak stars.
www.astrofilitrentini.it /mat/costell/aur_e.html   (423 words)

  
 eSky: Hoedus I
Though it is extremely luminous, it is also very distant from Earth (nearly 800 light years), and so it only appears to be of relatively faint magnitude, varying around +3.86.
This brief event causes the brightness of Hoedus I, as observed from Earth, to fall slightly.
Hoedus I is a winter star of the northern hemisphere, and like all the stars of its constellation Auriga, is most easily observed between November and January.
www.glyphweb.com /esky/stars/hoedusi.html   (151 words)

  
 COMMISSION 27 OF THE I
Zeta Aur is a prototype for a group of long period spectroscopic (and eclipsing) binary systems that consists of a K-type supergiant and a B-type main sequence companion.
The Zeta Aur system has been studied in detail since Harper (1924) first discovered it to be an ectipsing binary.
To investigate the nature of the photometric variations outside the eclipses of Zeta Aur, we have observed the system with UBV filters attached to the photoelectric photometer of the 30 cm Maksutov Telescope of Ankara University Observatory.
pluto.cc.ankara.edu.tr /~derman/dermanenglish/zetaaurigaeibovs89/zetaaurigaeibovs89.html   (456 words)

  
 Auriga (abbr. Aur, gen. Aurigae)
Epsilon Aurigae and Zeta Aurigae are remarkable eclipsing binaries.
Together with Eta Aur, they make up the so-called Kids, an asterism which lies just to the south and slightly ahead of Capella (whose name means the "She-Goat").
The most northerly of the trio, Epsilon, is a late addition; in antiquity Zeta and Eta were known respectively as "the western kid" and "the eastern kid."
www.daviddarling.info /encyclopedia/A/Aur.html   (300 words)

  
 Zeta AUR
Usually March and April are some of the clearest months in the year in Finland for observing stars so this was good opportunity to observe eclipse of zeta Aurigae.
It means zeta Aurigae appears to me normally (outside eclipse) as bright as 3.95 mag blue star.
Conclusions: With good luck it is possible even for single observer to measure zeta Aurigae minimum but uniting observations from different observers to single proper curve might be hard task due to red colour of variable and different red-sensitive eyes of observers.
www.student.oulu.fi /~ktikkane/AST/ZETAAUR.html   (570 words)

  
 Haedus I   (Site not responding. Last check: 2007-10-11)
Almaaz) is excluded, the term belonging to the bottom two, in Latin known as the "Haedi," the eastern (and faintest of the set) one now called Haedus I, the western Haedus II.
At bright fourth magnitude (3.75), Haedus I is the fainter of the pair (indeed of the three), though only because it is -- at a distance of 850 light years -- the farther.
Every 2.66 years, the smaller but still-bright B star hides completely behind the larger, cooler K star, and the combined visual light drops by 0.15 magnitudes (about 15 percent), not much, but noticeable to the practiced eye.
www.astro.uiuc.edu /~kaler/sow/haedus1.html   (423 words)

  
 Zeta Aurigae   (Site not responding. Last check: 2007-10-11)
The zeta Aurigae star system is a 6th magnitude system with a period of 2.7 years.
Because of the vast difference in sizes, only the primary eclipse where the orange super giant passes in front of the smaller blue star, is observable.
Along with the other star systems listed here, the zeta Aurigae system allows observations of the chromospheric, or outermost layers, of the orange super giant star.
www.hposoft.com /Astro/PEP/ZetaAurigae.html   (162 words)

  
 The Chromosphere and Wind of \zeta Aurigae   (Site not responding. Last check: 2007-10-11)
The \zeta Aurigae binary systems consist of evolved supergiants which eclipse their early-type main sequence companions.
To this end, we have undertaken an analysis of the chromosphere and wind of the prototype system, \zeta Aurigae, and we graphically demonstrate the resulting model by means of a video presentation.
Our atmospheric model of the chromosphere and wind of the primary star of \zeta Aurigae (K4 Ib + B5 V) is based on Cycle 2 and recent Cycle 5 observations obtained with the Goddard High Resolution Spectrograph (GHRS) aboard the Hubble Space Telescope, and on archival IUE and optical spectra.
www.aas.org /publications/baas/v27n4/aas187/S103004.html   (305 words)

  
 Current Projects   (Site not responding. Last check: 2007-10-11)
Observations of the eclipsing binary system zeta Aurigae with the Hubble Space Telescope Goddard High Resolution Spectrograph (GHRS).
Modeling the wind variability in zeta Aur as observed over the 17 year lifetime of the IUE satellite.
We propose that the intense Extended Red Emission (ERE) seen in the Red Rectangle Nebula around HD 44179 is due to decay of selected levels of excited triplet (mainly the "d") states to the metastable "a" state.
casa.colorado.edu /~pbennett/projects.html   (217 words)

  
 Capella: Alpha Aurigae   (Site not responding. Last check: 2007-10-11)
Alpha Aurigae is better known as Capella, the most northerly first-magnitude star.
The most northerly of these stars -- epsilon -- is a late addition; in antiquity zeta and eta were known respectively as "the western kid" and "the eastern kid".
Delta Aurigae isn't interesting in itself, but this part of Auriga brushes up against one of the more difficult ones -- Camelopardalus -- so you'll be coming back here when you study that constellation.
www.dibonsmith.com /aur_a.htm   (294 words)

  
 Auriga
Auriga's stars are fairly bright; five are second magnitude or brighter.
Auriga has three Messier objects: M36, M37, and M38.
M37 is the most spectacular of the three Messiers, and also the most easily found, as it lies midway between El Nath and theta Aurigae.
www.dibonsmith.com /aur_con.htm   (673 words)

  
 The Salopian Web - Constellations: Auriga
One of the brightest and largest constellations in the northern hemisphere, located to the west of Perseus,and above Taurus.
There is no Gamma Aurigae, since this, more properly, belongs to the constellation of Taurus, and is listed as Beta Taurus
It is thought that Auriga may represent the sea god Poseidon (Neptune), riding his chariot drawn by sea horses.
www.r-clarke.org.uk /constellations/auriga.htm   (126 words)

  
 SVIBOR - Papers - project code: 1-04-157
Zeta Aurigae are binaries composed of a late type supergiant and a smaller hot companion.
Degree level: M.A. Summary: Epsilon Aurigae is an eclipting binary of a Zeta Aur type.
According to the present model it is composed of two hot stars of spectral type O, the more massive one being surrounded by a dust and gas shell, while around the less massive component an accretion disc has been formed.
www.mzos.hr /svibor/1/04/157/rad_e.htm   (881 words)

  
 Auriga   (Site not responding. Last check: 2007-10-11)
Auriga was protrayed as a charioteer who was seen carying two to three children on his arm.
He was also known as Erechtheus, son of Hephaestus (Called Vulcan by the Romans).
Hephaestus, who was crippled as a child, was believed to have invented the chariot for his who created it so that his son could move him about more easily.
www.astro.wisc.edu /~dolan/constellations/constellations/Auriga.html   (60 words)

  
 Epsilon Aurigae, Campaign 2009
Epsilon Aurigae, a bright third-magnitude star in the northern sky, has puzzled astronomers for most of the last century.
Intereclipse Spectroscopic Snapshot of epsilon Aurigae with the Hubble Space Telescope, Sheffer and Lambert, 1999 PASP 111:829.
We suggest that the invisible companion in EE Cep is a dark, thick disc around a low-luminosity central star or binary, and that the system has a few important similarities to the epsilon Aur system.
www.du.edu /~rstencel/epsaur.htm   (1318 words)

  
 Multiple Systems
Zeta Aurigae Systems - Long period binaries comprising interacting type G or K supergiant and hot (~type B) companion.
VV Cephei Systems - Similar to Zeta Aurigae binaries except a type M supergiant replaces the G or K type.
Symbiotic Binaries - Long period (~200 to 1500 days) interacting binaries comprising a cool type M giant (sometimes a pulsating Mira-type variable) and a hot accreting companion such as a white dwarf, sub-dwarf, or low-mass main sequence star.
www.peripatus.gen.nz /Astronomy/MulSys.html   (421 words)

  
 [No title]
The slow passage of the geometrically small B dwarf with its bright UV continuum behind the extended atmosphere of the K supergiant provides a splendid opportunity to probe the column densities and velocities of many absorption lines of various strengths as a function of stellar impact parameter.
The continnuum of the B dwarf secondary of Zeta Aur is prominent only in the ultraviolet and data required for this program are not therefore obtainable from the ground.
Synthetic spectra calculated from these models will be compared with the observations and used to deduce the actual structure of the stellar atmosphere.
ecf.hq.eso.org /poa/FOS/props/5069c.pro   (1638 words)

  
 Weird Neighbors - Bad Astronomy and Universe Today Forum
The programs proposed and accepted for observations are therefore driven by scientists' interests, and the scientific merits of the proposals.
Spitzer will be no use for observing Epsilon Aurigae in August 2009, it will have run out of coolant before then.
Of course, NASA may decide that, in contrast to Hubble, Spitzer is worth a rescue/service mission.
www.bautforum.com /showthread.php?t=26792   (627 words)

  
 Almaaz   (Site not responding. Last check: 2007-10-11)
These contents are the property of the author and are reproduced from original without the author's express consent because of fair use and valid educational purposes.
Tucked to the southwest of Capella in Auriga is a prominent narrow triangle of stars.
The prototype eclipser, Algol (in Perseus), dims by about a magnitude every 2.87 days when a class K giant star passes in front of a small but bright hot class B star.
www.erectus.it /namedstars/almaaz.html   (473 words)

  
 [No title]
"The lower chromosphere of zeta Aurigae", K.-P. Schroeder, R.E.M. Griffin, R.F. Griffin, 1990, A&A 234, 299-307
"Chromospheric density distribution, opacity, ionization and wind acceleration of three K supergiants in zeta Aurigae systems", K.-P. Schroeder, 1987, in: 'Circumstellar matter', Proceedings of the 122nd IAU Symp., I. Appenzeller, C. Jordan (eds.), Reidel Publ.
"The technique of spectral subtraction: optical spectra of the chromosphere of zeta Aur", R.E.M. Griffin, R.F. Griffin, K.-P. Schroeder, 1990, 6th Cambridge workshop on cool stars, stellar systems and the sun, G.
astronomy.sussex.ac.uk /~kps/papers.htm   (2017 words)

  
 EOU-JOEL EATON
magnetic activity in cool stars, outer atmospheres of cool giant stars, eclipsing binary stars, zeta Aurigae binary stars, automating astronomical observation spots on chromospherically active cool stars.
Empirical models of atmospheres of cool stars derived from zeta Aurigae binaries.
Construction of a 2-meter automatic spectroscopic telescope to obtain high- and low-dispersion optical spectra of stars to 11th magnitude completely under computer control.
explorers.tsuniv.edu /People/JEATON.ASP   (83 words)

  
 [No title]
The slow line_3: passage of the geometrically small B dwarf with its bright UV continuum line_4: behind the extended atmosphere of the K supergiant provides a splendid line_5: opportunity to probe the column densities and velocities of many line_6: absorption lines of various strengths as a function of stellar impact line_7: parameter.
question: 4 section: 1 line_1: The continnuum of the B dwarf secondary of Zeta Aur is prominent only line_2: in the ultraviolet and data required for this program are not therefore line_3: obtainable from the ground.
Synthetic spectra calculated from these models will be line_15: compared with the observations and used to deduce the actual structure line_16: of the stellar atmosphere.
ecf.hq.eso.org /poa/FOS/props/3626c.prop   (2481 words)

  
 (IAAC) RE: Partial Listing of Asterisms and Some Comments
Centred on 14h51.0' -66O 12' is another brighter asterism that my friend's 14-years old daughter Alexandra Popovic coins 'The Golden Horseshoe.' It lies between Alpha () Circini and Gamma () Triangulum Australis, and some two-thirds the bisected distance in a straight line between these stars.
To the naked eye the brightest star in the asterism is the 6.2 magnitude bluish Zeta () Circini (SAO252951).
The Golden Horseshoe has a diameter c.0.8 degrees and contains some 25 stars - three of 6th magnitude, six are 7th, eleven of 8th and five of 9th.
www.visualdeepsky.org /netastrocatalog-announce/msg01235.html   (2071 words)

  
 MNRAS, 289, 869-881 (1997)   (Site not responding. Last check: 2007-10-11)
We present a detailed quantitative comparison of these fundamental data with evolution models for single stars computed with our evolution code, both with and without the effects of enhanced mixing or overshooting beyond the convective cores.
We use the same prescription for overshooting that Schröder, Pols & Eggleton found to reproduce the properties of zeta Aurigae binaries.
For about 80 per cent of the 49 binary systems in the sample, both sets of models provide a good fit to both stars at a single age and metallicity within the observational uncertainties.
www.phys.uu.nl /~pols/papers/evtesteb.html   (399 words)

  
 FAR ULTRAVIOLET SPECTROSCOPIC EXPLORER (FUSE)
These quantities can then be directly compared to values derived for the Milky Way through the O VI Program.
Zeta Aurigae/VV Cep eclipsing binary systems offer the most detailed method of studying mass loss from cool supergiant stars.
The FUV continuum from the hot main-sequence secondary star provides a probe through the outer atmosphere and wind of the evolved primary star.
research.hq.nasa.gov /code_s/nra/current/NRA-00-OSS-05/apendixg.html   (6616 words)

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