November, 2015 - The Baton Rouge Astronomical Society
... and 1 ½ ° east of Eta Piscium. Due to its large size and low surface brightness, M 74 is an elusive object to see. Two supernovae have been observed in M 74, SN 2002ap, and SN 2003gd. Sn2002ap was one of the rare Type 1C supernovae, also known as hyper-novae – super novae explosions with a substanti ...
... and 1 ½ ° east of Eta Piscium. Due to its large size and low surface brightness, M 74 is an elusive object to see. Two supernovae have been observed in M 74, SN 2002ap, and SN 2003gd. Sn2002ap was one of the rare Type 1C supernovae, also known as hyper-novae – super novae explosions with a substanti ...
Rotational Doppler beaming in eclipsing binaries
... systems where tidal forces are strong enough to synchronize the system, will be set by the synchronisation velocity vsync = P2πR . In wide binaries where tidal synorb chronization is ineffective, there is no hard lower limit to the rotational velocity of each of the components. In these equations M ...
... systems where tidal forces are strong enough to synchronize the system, will be set by the synchronisation velocity vsync = P2πR . In wide binaries where tidal synorb chronization is ineffective, there is no hard lower limit to the rotational velocity of each of the components. In these equations M ...
The ISO–SWS Spectrum of Planetary Nebula NGC 7027
... C HAPTER 2: The ISO–SWS Spectrum of Planetary Nebula NGC 7027 ...
... C HAPTER 2: The ISO–SWS Spectrum of Planetary Nebula NGC 7027 ...
P - Inaf
... Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies as functions of stellar and halo mass, with central and satellite galaxies in grey and black, respectively. The vertical bars in the left-hand panels indicate the typical ±1σ scatter in the model. For compa ...
... Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies as functions of stellar and halo mass, with central and satellite galaxies in grey and black, respectively. The vertical bars in the left-hand panels indicate the typical ±1σ scatter in the model. For compa ...
arXiv:1705.00964v1 [astro-ph.GA] 2 May 2017
... PKS1257-326 leave no doubt that the scattering material must be located at line-of-sight distances 1 kpc from us (Dennett-Thorpe and de Bruyn 2000, 2003). Thus a deep stellar catalogue is not necessary for crossmatching; we employ the Hipparcos catalogue (Perryman et al 1997). Figure 1 shows the l ...
... PKS1257-326 leave no doubt that the scattering material must be located at line-of-sight distances 1 kpc from us (Dennett-Thorpe and de Bruyn 2000, 2003). Thus a deep stellar catalogue is not necessary for crossmatching; we employ the Hipparcos catalogue (Perryman et al 1997). Figure 1 shows the l ...
binary stars instructor notes
... consisting of two stars, both classified as spectral type G5 V with magnitudes V = 6.26 and V = 6.36, having an orbital period of P = 25.0 years and a semi-major axis a = 0".67. Assume bolometric corrections of BC = –0.05 for G5 V stars and that the system is close enough to be unreddened by ...
... consisting of two stars, both classified as spectral type G5 V with magnitudes V = 6.26 and V = 6.36, having an orbital period of P = 25.0 years and a semi-major axis a = 0".67. Assume bolometric corrections of BC = –0.05 for G5 V stars and that the system is close enough to be unreddened by ...
A new view of galaxy evolution
... star formation, a common process in the early galaxies in the universe. universe. However, there are also galaxies that We are also now able to measure the amount are more “quiescent” or “passive” – not actively of mass in a galaxy which is in the form of forming stars – and these galaxies are much ...
... star formation, a common process in the early galaxies in the universe. universe. However, there are also galaxies that We are also now able to measure the amount are more “quiescent” or “passive” – not actively of mass in a galaxy which is in the form of forming stars – and these galaxies are much ...
Surface Gravity as a Diagnostic ... Youth Cameron Higby-Naquin Advisor: Eric Jensen
... Knowing the age of a star is only the first step to understanding stellar evolution and completely describing how stars change with time. In short, different stars take different amounts of time to form, and to fully grasp the formation process, physical properties of the star must be determined. A ...
... Knowing the age of a star is only the first step to understanding stellar evolution and completely describing how stars change with time. In short, different stars take different amounts of time to form, and to fully grasp the formation process, physical properties of the star must be determined. A ...
StellarManual
... An incomplete sentence is presented that indicates the size and surface temperature a certain star has relative to the Sun. Students should determine how the stellar luminosity will compare with the Sun. Initially there is no equation displayed. Answer: Luminosity of a star is proportional to the sq ...
... An incomplete sentence is presented that indicates the size and surface temperature a certain star has relative to the Sun. Students should determine how the stellar luminosity will compare with the Sun. Initially there is no equation displayed. Answer: Luminosity of a star is proportional to the sq ...
1. The Birth of a Star
... toward a faint colored cloud in space named “M42”. Notice that in the same info display, the distance from you to that cloud is listed as 1,177.7 ly. The “ly” stands for “Light Year”. It is not a time, but a distance. It is the distance a beam of light will travel through space in one year. 13. Ligh ...
... toward a faint colored cloud in space named “M42”. Notice that in the same info display, the distance from you to that cloud is listed as 1,177.7 ly. The “ly” stands for “Light Year”. It is not a time, but a distance. It is the distance a beam of light will travel through space in one year. 13. Ligh ...
Absolute magnitudes and kinematics of barium
... (Jorissen & Boffin 1992) and that the orbital period is related to the orbital separation. It may be possible that mild barium stars have wider separations between components, making more difficult the detection of their binary nature. If we consider the stars with known orbits or with variable radi ...
... (Jorissen & Boffin 1992) and that the orbital period is related to the orbital separation. It may be possible that mild barium stars have wider separations between components, making more difficult the detection of their binary nature. If we consider the stars with known orbits or with variable radi ...
FIRST STELLAR ABUNDANCES IN THE DWARF IRREGULAR
... The analysis of bright nebular emission lines of H II regions has been the most frequent approach to modeling chemical evolution of more distant galaxies to date (Matteucci & Tosi 1985). So far, only a very limited number of elements can be examined and quantified when using this approach. The chemi ...
... The analysis of bright nebular emission lines of H II regions has been the most frequent approach to modeling chemical evolution of more distant galaxies to date (Matteucci & Tosi 1985). So far, only a very limited number of elements can be examined and quantified when using this approach. The chemi ...
The Milky Way disk
... Center, we can obtain precise information -both from ground and with dedicated satellites- for many individual stars, star clusters, and molecular clouds. However, this does not represent always a real advantage when we try do derive general properties of galactic components, e.g. the bulge, the hal ...
... Center, we can obtain precise information -both from ground and with dedicated satellites- for many individual stars, star clusters, and molecular clouds. However, this does not represent always a real advantage when we try do derive general properties of galactic components, e.g. the bulge, the hal ...
Astronomy 250 - University of Victoria
... though a star’s movement across the sky (its proper motion, often given in arcseconds per year) can be measured. Proper motions are generally measured by taking two pictures of a stellar field a few years apart. The change in position and direction of motion of a given star can be determined by meas ...
... though a star’s movement across the sky (its proper motion, often given in arcseconds per year) can be measured. Proper motions are generally measured by taking two pictures of a stellar field a few years apart. The change in position and direction of motion of a given star can be determined by meas ...
Red supergiants around the obscured open cluster Stephenson 2
... (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our targets present a good quality flag (Qflg = A, B, C, or D) in all three 2MASS bands. A few objects with other quality flags were included in the sample and assigned low priori ...
... (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our targets present a good quality flag (Qflg = A, B, C, or D) in all three 2MASS bands. A few objects with other quality flags were included in the sample and assigned low priori ...
Galaxies
... Edwin Hubble noticed that there were Cepheid variable stars in the Andromeda “nebula” Using the luminosity, period relation for Cepheids and the measured luminosity, he showed that the Andromeda system was far outside of the Milky Way Hubble did similar studies with respect to many of the other “neb ...
... Edwin Hubble noticed that there were Cepheid variable stars in the Andromeda “nebula” Using the luminosity, period relation for Cepheids and the measured luminosity, he showed that the Andromeda system was far outside of the Milky Way Hubble did similar studies with respect to many of the other “neb ...
A Spectroscopic Survey of a Sample of Active M Dwarfs.
... their published velocities (Marcy, Lindsay & Wilson 1987) subtracted. The standard deviation, with no corrections applied other than the standard heliocentric ones, is 1.2 km s−1 , and the formal mean is −0.1 km s−1 . Our observations are listed in Table 1. Column 1 is the full RASS designation of e ...
... their published velocities (Marcy, Lindsay & Wilson 1987) subtracted. The standard deviation, with no corrections applied other than the standard heliocentric ones, is 1.2 km s−1 , and the formal mean is −0.1 km s−1 . Our observations are listed in Table 1. Column 1 is the full RASS designation of e ...
The Korean 1592--1593 Record of a Guest Star: Animpostor`of the
... star that appeared very close to Cas A was made by Korean astronomers in 1592–1593, for which Brosche (1967) and Chu (1968) independently proposed that it might have been the Cas A SN event. On the other hand, Stephenson & Yau (1987) (see also Stephenson & Green 2002, for a summary), who studied thi ...
... star that appeared very close to Cas A was made by Korean astronomers in 1592–1593, for which Brosche (1967) and Chu (1968) independently proposed that it might have been the Cas A SN event. On the other hand, Stephenson & Yau (1987) (see also Stephenson & Green 2002, for a summary), who studied thi ...
bars and secular evolution
... (i) how such disks can form (the angular momentum problem) (ii) how they survive without going unstable and forming bulges - role of the dark halo, anisotropy limits ... Exciting field - serious problems - much work to do in observations, dynamical theory, galaxy formation theory ... ...
... (i) how such disks can form (the angular momentum problem) (ii) how they survive without going unstable and forming bulges - role of the dark halo, anisotropy limits ... Exciting field - serious problems - much work to do in observations, dynamical theory, galaxy formation theory ... ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... This course introduces you to the bright stars and major constellations visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a s ...
... This course introduces you to the bright stars and major constellations visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a s ...
Epsilon Aurigae: a rare stellar eclipse - Project VS
... system of epsilon Aurigae. Using an instrument developed at the University of Michigan, scientists have taken close-up pictures of Epsilon Aurigae during its eclipse. A series of images obtained at the Center for High Angular Resolution interferometer with the Michigan Infrared beam Combiner (CHARA- ...
... system of epsilon Aurigae. Using an instrument developed at the University of Michigan, scientists have taken close-up pictures of Epsilon Aurigae during its eclipse. A series of images obtained at the Center for High Angular Resolution interferometer with the Michigan Infrared beam Combiner (CHARA- ...
Lecture 2 Astronomical Distances
... ≈ → V ≈ 600 km s −1 T c Largely due to Milky Way (Local Group) falling toward Virgo Cluster. ...
... ≈ → V ≈ 600 km s −1 T c Largely due to Milky Way (Local Group) falling toward Virgo Cluster. ...
Abstracts - Physics of Evolved Stars 2015
... During the past decade, an increasing number of observations have shown that, at least at some points, the mass-loss rate of red supergiants (RSG) could be significantly higher than the standard one, usually used in stellar evolution code. In this talk, I will show how an increased mass-loss rate du ...
... During the past decade, an increasing number of observations have shown that, at least at some points, the mass-loss rate of red supergiants (RSG) could be significantly higher than the standard one, usually used in stellar evolution code. In this talk, I will show how an increased mass-loss rate du ...
On the Spiral Structure of the Milky Way Galaxy
... Data on other galaxies are known to demonstrate that HI superclouds, giant molecular clouds (GMCs) and young stars genetically related to them, and HII regions are located along spiral arms and often concentrated in giant star and gas complexes [5, 6]. The complexes in the spiral arms related to the ...
... Data on other galaxies are known to demonstrate that HI superclouds, giant molecular clouds (GMCs) and young stars genetically related to them, and HII regions are located along spiral arms and often concentrated in giant star and gas complexes [5, 6]. The complexes in the spiral arms related to the ...
sections 19-22 instructor notes
... The maximum and/or minimum observed radial velocities of hydrogen clouds along such lines of sight in the 1st and 4th quadrants, respectively, must originate from gas located at the tangent points, if there is any. In general terms there will always be some hydrogen gas at the tangent points, but t ...
... The maximum and/or minimum observed radial velocities of hydrogen clouds along such lines of sight in the 1st and 4th quadrants, respectively, must originate from gas located at the tangent points, if there is any. In general terms there will always be some hydrogen gas at the tangent points, but t ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.