Luminosities and mass-loss rates of SMC and LMC AGB stars and
... The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
... The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
LCM SerieS
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
Stars and Planets Credits and Acknowledgements
... make a scale model of time rather than distance. The lifetimes of different masses of stars are compared to each other and to the geologic timeline for the Earth. Students then make predictions about what classes of main sequence stars might have planets with interesting life forms (as defined by th ...
... make a scale model of time rather than distance. The lifetimes of different masses of stars are compared to each other and to the geologic timeline for the Earth. Students then make predictions about what classes of main sequence stars might have planets with interesting life forms (as defined by th ...
Extrasolar Planet Studies:The Italian Contribution
... very similar late-F early-G stars (where the convective envelope is tiny) ...
... very similar late-F early-G stars (where the convective envelope is tiny) ...
Asteroid Rotation Periods
... Early brightness measurements of asteroids revealed both periodic timedependent variations and a phenomenon called the opposition effect (this is the sudden rise of the asteroid’s brightness when it’s very close to opposition). However, from photometric measurements in the visual wavelengths alone, ...
... Early brightness measurements of asteroids revealed both periodic timedependent variations and a phenomenon called the opposition effect (this is the sudden rise of the asteroid’s brightness when it’s very close to opposition). However, from photometric measurements in the visual wavelengths alone, ...
The science case for - Astrophysics
... cold dark matter scenario. Snapshots are shown at various times from the early Universe (z=50) to the present day (z=0). Primary science cases for a 50metre-100metre Extremely Large Telescope Are there terrestrial planets orbiting other stars? Are we alone? Direct detection of earth-like planets in ...
... cold dark matter scenario. Snapshots are shown at various times from the early Universe (z=50) to the present day (z=0). Primary science cases for a 50metre-100metre Extremely Large Telescope Are there terrestrial planets orbiting other stars? Are we alone? Direct detection of earth-like planets in ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
SPIRou Science Case
... search for & characterize habitable exo-Earths orbiting low-mass & very-low mass stars (LMSs & vLMSs) using high-precision radial velocity (RV) measurements. This search will expand the initial, exploratory studies carried out with visible instruments (e.g., HARPS/ESO) and will survey in particular ...
... search for & characterize habitable exo-Earths orbiting low-mass & very-low mass stars (LMSs & vLMSs) using high-precision radial velocity (RV) measurements. This search will expand the initial, exploratory studies carried out with visible instruments (e.g., HARPS/ESO) and will survey in particular ...
X-Ray Properties of Young Stars and Stellar Clusters
... X-ray emission and flaring is thus ubiquitous in PMS stars across the initial mass function (IMF). The X-ray luminosity function (XLF) is broad, spanning 28 < log L x[erg/ s] < 32 (0.5–8 keV), with a peak around log L x[erg/s] ~ 29 (Feigelson et al., 2005). For comparison, the contemporary Sun emits ...
... X-ray emission and flaring is thus ubiquitous in PMS stars across the initial mass function (IMF). The X-ray luminosity function (XLF) is broad, spanning 28 < log L x[erg/ s] < 32 (0.5–8 keV), with a peak around log L x[erg/s] ~ 29 (Feigelson et al., 2005). For comparison, the contemporary Sun emits ...
The low-mass dispersed population around the Lupus clouds
... and 4), providing diagnostic features of temperature and surface gravity as well as accretion/outflow diagnostic lines near Hα. It also includes the LiI line at 6708 Å, but unfortunately the combination of resolution and signal-to-noise ratio of our spectra provide only upper limits of no practical ...
... and 4), providing diagnostic features of temperature and surface gravity as well as accretion/outflow diagnostic lines near Hα. It also includes the LiI line at 6708 Å, but unfortunately the combination of resolution and signal-to-noise ratio of our spectra provide only upper limits of no practical ...
PDF 523 KB
... All the area of the sky around the ecliptic was being photographed, down to magnitude 16 ( stars almost 10000 times fainter than the dimmest stars visible by the naked eye ). The pictures were later scanned with use of the so called “blink comparator” during the day. The idea was, that if there was ...
... All the area of the sky around the ecliptic was being photographed, down to magnitude 16 ( stars almost 10000 times fainter than the dimmest stars visible by the naked eye ). The pictures were later scanned with use of the so called “blink comparator” during the day. The idea was, that if there was ...
Downloaded - Royal Society Open Science
... Decades of unsuccessful attempts to find planets around other Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around the millisecond pulsar PSR B1257+12 were the first confidently reported extrasolar planets to withstand enduring s ...
... Decades of unsuccessful attempts to find planets around other Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around the millisecond pulsar PSR B1257+12 were the first confidently reported extrasolar planets to withstand enduring s ...
Article PDF - IOPscience
... we considered here only stars that were hot enough for the spectroscopic method to be reliable, Teff 6500 K). There are also several DB stars in the spectroscopic analysis of Bergeron et al. (2011) with distances within 20 pc, although all of these lie in a temperature regime where the physics of ...
... we considered here only stars that were hot enough for the spectroscopic method to be reliable, Teff 6500 K). There are also several DB stars in the spectroscopic analysis of Bergeron et al. (2011) with distances within 20 pc, although all of these lie in a temperature regime where the physics of ...
A Spitzer mid-infrared spectral survey of mass
... source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright oxygen-rich object near (J − K , M K ) ∼ (1, −10.7) in Fig. 1(b) was not a target but was accidentally observed when Spitzer sel ...
... source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright oxygen-rich object near (J − K , M K ) ∼ (1, −10.7) in Fig. 1(b) was not a target but was accidentally observed when Spitzer sel ...
On the elemental abundance and isotopic mixture of mercury in
... on the behaviour of the Hg λ3984 line, but the latter two studied the Hg λ4358 line in selected stars. Smith (1997) also included a low-resolution study of Hg λ1942 using data from the International Ultraviolet Explorer (IUE) satellite. High-resolution ultraviolet studies of additional mercu ...
... on the behaviour of the Hg λ3984 line, but the latter two studied the Hg λ4358 line in selected stars. Smith (1997) also included a low-resolution study of Hg λ1942 using data from the International Ultraviolet Explorer (IUE) satellite. High-resolution ultraviolet studies of additional mercu ...
Untitled - METU Astrophysics Home Page
... Applicability of the Models to Data from Accretion Powered X-Ray Sources . . . . . . . . . . ...
... Applicability of the Models to Data from Accretion Powered X-Ray Sources . . . . . . . . . . ...
Evolution of low mass stars
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
Open clusters and associations in the Gaia era
... an issue if the survey does not extend beyond the cluster tidal radius, especially if there is mass segregation as the incompleteness level will then depend on mass. Moreover, objects might be missed around bright stars due to contrast issue, in crowded regions or in area with high extinction. As fo ...
... an issue if the survey does not extend beyond the cluster tidal radius, especially if there is mass segregation as the incompleteness level will then depend on mass. Moreover, objects might be missed around bright stars due to contrast issue, in crowded regions or in area with high extinction. As fo ...
Where stars form: inside-out growth and coherent star formation from
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.