Rotation Periods and Relative Ages of Solar-Type Stars
... on axes of log Teff (effective temperature) and δMbol (bolometric luminosity). Also, Ca II H (396.8 nm) and K (383.4 nm) chromospheric emissions are empirically linked to ages (Soderblom et al. 1991). By fitting Strömgren uvby-Hβ photometry data to theoretical isochrones, isochrone ages may be compa ...
... on axes of log Teff (effective temperature) and δMbol (bolometric luminosity). Also, Ca II H (396.8 nm) and K (383.4 nm) chromospheric emissions are empirically linked to ages (Soderblom et al. 1991). By fitting Strömgren uvby-Hβ photometry data to theoretical isochrones, isochrone ages may be compa ...
Sparse aperture masking at the VLT II. Detection limits for the eight
... tems2 . Other evolutionary models do exist and are based on similar or alternative planet formation scenarios, such as the ’warm-start’ model proposed by Spiegel & Burrows (2012). The mass/luminosity isochrones derived from other models can be perfectly applied to the data we made available online. ...
... tems2 . Other evolutionary models do exist and are based on similar or alternative planet formation scenarios, such as the ’warm-start’ model proposed by Spiegel & Burrows (2012). The mass/luminosity isochrones derived from other models can be perfectly applied to the data we made available online. ...
The Final Version of the White Paper is available.
... absorption lines of our atmosphere and to increase detection capability by allowing the detection of narrow lines, but also to trace different layers of the atmosphere and exoplanet weather), a wide wavelength range (0.37-2.5 µm), high stability of the PSF on the detector during planetary transits a ...
... absorption lines of our atmosphere and to increase detection capability by allowing the detection of narrow lines, but also to trace different layers of the atmosphere and exoplanet weather), a wide wavelength range (0.37-2.5 µm), high stability of the PSF on the detector during planetary transits a ...
Evidence for the Tidal Destruction of Hot Jupiters by Subgiant Stars
... Milky Way, and empirically it is known that the velocity dispersion of a thin-disk population increases with age (e.g., Binney et al. 2000). This is understood as follows. Thin disk stars form from dense, turbulent gas in the Galactic plane. Because that process is highly dissipative, stellar popula ...
... Milky Way, and empirically it is known that the velocity dispersion of a thin-disk population increases with age (e.g., Binney et al. 2000). This is understood as follows. Thin disk stars form from dense, turbulent gas in the Galactic plane. Because that process is highly dissipative, stellar popula ...
Introduction
... some exoplanets. With the latter, polar or retrograde planet orbits can be identified. However, as the inclinations are degenerate over the inclination to the plane of the sky, it is not possible to compare them to the values in the Solar System or in the planet formation and evolution models. So fa ...
... some exoplanets. With the latter, polar or retrograde planet orbits can be identified. However, as the inclinations are degenerate over the inclination to the plane of the sky, it is not possible to compare them to the values in the Solar System or in the planet formation and evolution models. So fa ...
Chemical analysis of 24 dusty (pre-) main
... as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display emission lines, and illuminate a bright reflection nebula in their immediate vicinity. Later on other observational criteria were proposed. Finkenzeller & Mundt (1984) mentioned th ...
... as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display emission lines, and illuminate a bright reflection nebula in their immediate vicinity. Later on other observational criteria were proposed. Finkenzeller & Mundt (1984) mentioned th ...
XRaySNR_sm - Gettysburg College
... Student Handout ............................................................................................................................................................... 13 The XMM-Newton Observatory .............................................................................................. ...
... Student Handout ............................................................................................................................................................... 13 The XMM-Newton Observatory .............................................................................................. ...
Starburst Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org T Heckman
... luminosity of the starburst. Thus, another way to find starbursts is to search for galaxies with unusually bright emission lines. The dust grains in the starburst are effective at absorbing ultraviolet photons of all wavelengths. The grains are heated by this radiation and cool by emitting radiation ...
... luminosity of the starburst. Thus, another way to find starbursts is to search for galaxies with unusually bright emission lines. The dust grains in the starburst are effective at absorbing ultraviolet photons of all wavelengths. The grains are heated by this radiation and cool by emitting radiation ...
Small star patterns for telescopes and binoculars Demelza Ramakers
... Unfortunately I haven’t found the exact coordinates for all asterisms, but instead of that I described as good as possible where the object is located. Some asterisms are catalogued in the STAR-Catalogue, where STAR stands for Small Telescope Asterism Roster. The charts that I’ve used are all made w ...
... Unfortunately I haven’t found the exact coordinates for all asterisms, but instead of that I described as good as possible where the object is located. Some asterisms are catalogued in the STAR-Catalogue, where STAR stands for Small Telescope Asterism Roster. The charts that I’ve used are all made w ...
The Interstellar Medium White Paper
... gas has itself formed. But how do molecular clouds form in the first place? This fundamental process has yet to be observed. It is the rate-determining step for star formation itself. Observations of external spiral galaxies show that massive stars and their giant molecular clouds (GMCs) tend to for ...
... gas has itself formed. But how do molecular clouds form in the first place? This fundamental process has yet to be observed. It is the rate-determining step for star formation itself. Observations of external spiral galaxies show that massive stars and their giant molecular clouds (GMCs) tend to for ...
Brightness and Flux Density
... Astronomers learn about an astronomical source by measuring the strength of its radiation as a function of direction on the sky (by mapping or imaging) and frequency (spectroscopy), plus other quantities (time, polarization) that we ignore for now. We need precise and quantitative definitions to des ...
... Astronomers learn about an astronomical source by measuring the strength of its radiation as a function of direction on the sky (by mapping or imaging) and frequency (spectroscopy), plus other quantities (time, polarization) that we ignore for now. We need precise and quantitative definitions to des ...
Astronomy Astrophysics First detection of the field star overdensity in the Perseus... &
... suitable direction to undertake this study on Galactic structure and kinematics is towards the anticenter and the Perseus arm. First, this direction presents lower interstellar extinction than the direction pointing to the Galactic center. Second, although slightly depending on the pitch angle, this ...
... suitable direction to undertake this study on Galactic structure and kinematics is towards the anticenter and the Perseus arm. First, this direction presents lower interstellar extinction than the direction pointing to the Galactic center. Second, although slightly depending on the pitch angle, this ...
Characterization of the four new transiting planets KOI
... on the observation, we detected two sets of barely resolved spectral lines separated by a few km s−1 , or a unique set of spectral lines that we interpreted as the superposition of the two sets being located at a similar radial velocity at that time. The corresponding radial velocities and bisector ...
... on the observation, we detected two sets of barely resolved spectral lines separated by a few km s−1 , or a unique set of spectral lines that we interpreted as the superposition of the two sets being located at a similar radial velocity at that time. The corresponding radial velocities and bisector ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
... nine cool main-sequence dwarfs of the solar neighbourhood. The resolving power of the spectra was R ∼ 50 000 and the exposure times were chosen to achieve a signal-to-noise ratio (S/N) larger than 200. The reduction and calibration of the spectra were carried out with the standard CRIRES pipeline pr ...
... nine cool main-sequence dwarfs of the solar neighbourhood. The resolving power of the spectra was R ∼ 50 000 and the exposure times were chosen to achieve a signal-to-noise ratio (S/N) larger than 200. The reduction and calibration of the spectra were carried out with the standard CRIRES pipeline pr ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.