![Infrared Properties of Star-Forming Dwarf Galaxies. I. Dwarf Irregular](http://s1.studyres.com/store/data/016020349_1-496a7aac2297c069802ee97f5678be2a-300x300.png)
ppt
... photon noise, whereas the dashed line shows the corresponding dispersion for 10-point averages. For most objects, the dispersion of 10point averages is much higher than that which is expected for white noise, especially for brighter magnitudes. The dotted line shows the expected dispersion of the 10 ...
... photon noise, whereas the dashed line shows the corresponding dispersion for 10-point averages. For most objects, the dispersion of 10point averages is much higher than that which is expected for white noise, especially for brighter magnitudes. The dotted line shows the expected dispersion of the 10 ...
24.1 Hubble`s Galaxy Classification
... This pair of images shows the Coma cluster of galaxies. Almost every object visible is a galaxy. Coma Cluster (a) A collection of many galaxies, each consisting of hundreds of billions of stars. Called the Coma Cluster, this group of galaxies lies more than 100 million pc from Earth. (The blue spike ...
... This pair of images shows the Coma cluster of galaxies. Almost every object visible is a galaxy. Coma Cluster (a) A collection of many galaxies, each consisting of hundreds of billions of stars. Called the Coma Cluster, this group of galaxies lies more than 100 million pc from Earth. (The blue spike ...
Sample pages 1 PDF
... An attentive observer will soon notice that individual bright stars that are rather close together in the sky seem to form simple geometric shapes – squares, rhombuses, crosses, circles, arches. Giving a name to these shapes in the sky makes them more familiar to you and easier to locate again. That ...
... An attentive observer will soon notice that individual bright stars that are rather close together in the sky seem to form simple geometric shapes – squares, rhombuses, crosses, circles, arches. Giving a name to these shapes in the sky makes them more familiar to you and easier to locate again. That ...
here - NASA/IPAC Extragalactic Database
... stars to red supergiants, or the relative number of WC- and WN-type WRs. Secondly, these massive stars affect the overall evolution and properties of the galaxies themselves, through three “feedback” mechanisms (see, e.g., Oey & Clarke 2009). First, their ultraviolet radiation heats dust, powering t ...
... stars to red supergiants, or the relative number of WC- and WN-type WRs. Secondly, these massive stars affect the overall evolution and properties of the galaxies themselves, through three “feedback” mechanisms (see, e.g., Oey & Clarke 2009). First, their ultraviolet radiation heats dust, powering t ...
Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... Balmer Hα regions. The details of the several instrumental setups used are given in Table 3. Slits of 1 were used in all runs. Spectroscopic data were reduced using Starlink packages ccdpack (Draper et al. 2000) and figaro (Shortridge et al. 1997) using standard techniques. After correcting the im ...
... Balmer Hα regions. The details of the several instrumental setups used are given in Table 3. Slits of 1 were used in all runs. Spectroscopic data were reduced using Starlink packages ccdpack (Draper et al. 2000) and figaro (Shortridge et al. 1997) using standard techniques. After correcting the im ...
Rotation Periods and Relative Ages of Solar-Type Stars
... chromospheres of stars; starspots are greatest where magnetic fields are greatest. Hence, as starspots or inhomogeneities travel across the surface of a star, Ca II flux will reflect that movement (Donahue 1993). Ca II flux is thus used to observe rotation periods. The search for rotational signals ...
... chromospheres of stars; starspots are greatest where magnetic fields are greatest. Hence, as starspots or inhomogeneities travel across the surface of a star, Ca II flux will reflect that movement (Donahue 1993). Ca II flux is thus used to observe rotation periods. The search for rotational signals ...
Neon abundances - UCL Astrophysics Group
... Explorer (IUE) on the ultraviolet resonance lines of iron-peak elements in 26 HgMn, four superficially normal and 10 normal stars. We observed definite detections or determined upper limits for Ne i in 21 of the HgMn stars in the Smith & Dworetsky (1993) sample, and in 11 of the normal and superfici ...
... Explorer (IUE) on the ultraviolet resonance lines of iron-peak elements in 26 HgMn, four superficially normal and 10 normal stars. We observed definite detections or determined upper limits for Ne i in 21 of the HgMn stars in the Smith & Dworetsky (1993) sample, and in 11 of the normal and superfici ...
Finding KBO Flyby Targets for New Horizons
... Table I also shows the diameter, for two plausible values of KBO geometric albedo p, corresponding to the given KBO magnitudes at 42 AU, which is the most likely encounter distance according to our model (probability is reduced by the narrowness of the accessibility cone at closer distances, and by ...
... Table I also shows the diameter, for two plausible values of KBO geometric albedo p, corresponding to the given KBO magnitudes at 42 AU, which is the most likely encounter distance according to our model (probability is reduced by the narrowness of the accessibility cone at closer distances, and by ...
Astrophysics Pristine CNO abundances from Magellanic Cloud B stars
... Large Magellanic Cloud (LMC). Apart from H ii regions, unevolved OB-type stars are currently the only accessible source of present-day CNO abundances for the MCs not altered by stellar evolution. Using UVES on the VLT, we obtained spectra of sufficient resolution (R = 20 000) and signal-to-noise (S/ ...
... Large Magellanic Cloud (LMC). Apart from H ii regions, unevolved OB-type stars are currently the only accessible source of present-day CNO abundances for the MCs not altered by stellar evolution. Using UVES on the VLT, we obtained spectra of sufficient resolution (R = 20 000) and signal-to-noise (S/ ...
Sample pages 1 PDF
... nuclear physics is occurring. Therefore, most AGB stars are classified as M, R, N or S, designations that have mostly been replaced by a collective term C, or “carbon stars.” Such stars have an abundance of carbon or oxygen in their photospheres, as there is an exchange of material between the core a ...
... nuclear physics is occurring. Therefore, most AGB stars are classified as M, R, N or S, designations that have mostly been replaced by a collective term C, or “carbon stars.” Such stars have an abundance of carbon or oxygen in their photospheres, as there is an exchange of material between the core a ...
Celebrating Astronomy: The Life of a Star
... most influence how stars are formed? Consider: • Mass of the initial gas cloud • Temperature of the gas ...
... most influence how stars are formed? Consider: • Mass of the initial gas cloud • Temperature of the gas ...
preprint, pdf version - LESIA
... events observed in Brazil and Chile (4 June 2011) and in Hawaii (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of ...
... events observed in Brazil and Chile (4 June 2011) and in Hawaii (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of ...
Process of Science: PreMainSequence Stellar Life Tracks on the HR
... The Sun was much more luminous when it was a protostar than it is today. The Sun was cooler and dimmer when it was a protostar than it is today. The Sun was much hotter when it was a protostar than it is today. ...
... The Sun was much more luminous when it was a protostar than it is today. The Sun was cooler and dimmer when it was a protostar than it is today. The Sun was much hotter when it was a protostar than it is today. ...
MASSIVE CLOSE BINARIES
... that Case B is the more frequent class of interacting binaries. Compared to Case B, it is trivial to understand that Case A components have smaller final masses whereas it is obvious that Case C (and non-interacting) binaries are similar to single stars. Equation 1 decides upon the mass loss during ...
... that Case B is the more frequent class of interacting binaries. Compared to Case B, it is trivial to understand that Case A components have smaller final masses whereas it is obvious that Case C (and non-interacting) binaries are similar to single stars. Equation 1 decides upon the mass loss during ...
The Classification of Stellar Spectra
... Background: The History And Nature Of Spectral Classification Patterns of absorption lines were first observed in the spectrum of the sun by the German physicist Joseph von Fraunhofer early in the 1800’s, but it was not until late in the century that astronomers were able to routinely examine the sp ...
... Background: The History And Nature Of Spectral Classification Patterns of absorption lines were first observed in the spectrum of the sun by the German physicist Joseph von Fraunhofer early in the 1800’s, but it was not until late in the century that astronomers were able to routinely examine the sp ...
THE N/O RATIO IN EARLY B-TYPE MAIN SEQUENCE STARS AS
... This paper is based on previous studies of MS B-stars which were published between 2000 and 2008 by Lyubimkov, et al. [8-12]. High resolution spectra for more than 100 MS B-stars were obtained [8] at two observatories, the Crimean Astrophysical Observatory and the MacDonald Observatory of the Unive ...
... This paper is based on previous studies of MS B-stars which were published between 2000 and 2008 by Lyubimkov, et al. [8-12]. High resolution spectra for more than 100 MS B-stars were obtained [8] at two observatories, the Crimean Astrophysical Observatory and the MacDonald Observatory of the Unive ...
The empirical mass distribution of hot B subdwarfs
... is an indication that the majority of sdB stars, including the isolated ones, are indeed post-red giant stars. Moreover, the empirical mass distribution strongly peaking at ∼0.47 M suggests that, in most cases, helium ignition occurs in the stellar core through a He-flash. The peak at ∼0.47 M also ...
... is an indication that the majority of sdB stars, including the isolated ones, are indeed post-red giant stars. Moreover, the empirical mass distribution strongly peaking at ∼0.47 M suggests that, in most cases, helium ignition occurs in the stellar core through a He-flash. The peak at ∼0.47 M also ...
Homework #3, AST 1002
... Which of the following is (are) correct? (a) Energy is transported from the Sun's core to its surface primarily by a process called convection. (b) It takes about five minutes for energy from the Sun's core to reach its surface. (c) The proton cycle describes the process of energy production in the ...
... Which of the following is (are) correct? (a) Energy is transported from the Sun's core to its surface primarily by a process called convection. (b) It takes about five minutes for energy from the Sun's core to reach its surface. (c) The proton cycle describes the process of energy production in the ...
Boötes
![](https://en.wikipedia.org/wiki/Special:FilePath/Sidney_Hall_-_Urania's_Mirror_-_Bootes,_Canes_Venatici,_Coma_Berenices,_and_Quadrans_Muralis.jpg?width=300)
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.