A Practical Guide to Exoplanet Observing
... any binning of the CCD camera is considered, should be such that the full width at half maximum (FWHM) of the host star spans three (3) or more pixels. Unlike deep sky imaging where the imager is interested in pinpoint stars, exoplanet observing is more interested in collecting accurate information ...
... any binning of the CCD camera is considered, should be such that the full width at half maximum (FWHM) of the host star spans three (3) or more pixels. Unlike deep sky imaging where the imager is interested in pinpoint stars, exoplanet observing is more interested in collecting accurate information ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... Sandstrom et al. 2013). In regions of vigorous star formation, however, αCO decreases by a factor of several (e.g., Downes & Solomon 1998; Tacconi et al. 2008). As a further complication, the high-ΣSFR galaxies that are much more common at high redshift are rare in the local universe, which makes th ...
... Sandstrom et al. 2013). In regions of vigorous star formation, however, αCO decreases by a factor of several (e.g., Downes & Solomon 1998; Tacconi et al. 2008). As a further complication, the high-ΣSFR galaxies that are much more common at high redshift are rare in the local universe, which makes th ...
Astrometry of Asteroids
... In this exercise you will be using images of the sky to find asteroids and measure their positions. Asteroids are small rocky objects that orbit the sun just like planets. They are located predominately between the orbit of Mars and Jupiter, about 2.8 Astronomical Units from the sun. Asteroids do or ...
... In this exercise you will be using images of the sky to find asteroids and measure their positions. Asteroids are small rocky objects that orbit the sun just like planets. They are located predominately between the orbit of Mars and Jupiter, about 2.8 Astronomical Units from the sun. Asteroids do or ...
Teil 2
... orbital motion, i.e., they appear centred at the central meridian during the respective quadrature phases, thus are not facing each other as would be the case for a hypothetical reflection effect. The leading hemispheres on both components appear with an effectively lower temperature than the traili ...
... orbital motion, i.e., they appear centred at the central meridian during the respective quadrature phases, thus are not facing each other as would be the case for a hypothetical reflection effect. The leading hemispheres on both components appear with an effectively lower temperature than the traili ...
2 Statistical properties of a sample of periodically variable B-type supergiants
... Waelkens et al. (1998) remained the most valuable one to observationally investigate the occurrence of gravity modes in supergiant stars, because it is unbiased and not selected to be observed with HIPPARCOS on the basis of variability. For this reason, we conducted an extensive spectroscopic campai ...
... Waelkens et al. (1998) remained the most valuable one to observationally investigate the occurrence of gravity modes in supergiant stars, because it is unbiased and not selected to be observed with HIPPARCOS on the basis of variability. For this reason, we conducted an extensive spectroscopic campai ...
GALEX and Star Formation
... colors). However, for UV-steeper extinction curves, such as LMC- and SMC-like curves, which are typical of young starburst regions, the FUV increase of the absorption Aλ is larger, and the 2175Å extinction “bump” less pronounced, making the observed FUV−NUV color highly sensitive to the amount, and ...
... colors). However, for UV-steeper extinction curves, such as LMC- and SMC-like curves, which are typical of young starburst regions, the FUV increase of the absorption Aλ is larger, and the 2175Å extinction “bump” less pronounced, making the observed FUV−NUV color highly sensitive to the amount, and ...
The Perseid Meteor Shower
... could see it. Comet Swift-Tuttle is about 8 kilometers (5 miles) in diameter. It takes 135 years to orbit our Sun and will not fly by Earth again until the year 2126. On August 12, Earth will fly through part of the dust tail of Comet Swift-Tuttle. Comet Swift-Tuttle won't be nearby, but there will ...
... could see it. Comet Swift-Tuttle is about 8 kilometers (5 miles) in diameter. It takes 135 years to orbit our Sun and will not fly by Earth again until the year 2126. On August 12, Earth will fly through part of the dust tail of Comet Swift-Tuttle. Comet Swift-Tuttle won't be nearby, but there will ...
Optical Spectroscopy of a Flare on Barnard`s Star
... of enhanced features, including the Balmer series, during a flare event that we observed which is significantly stronger than the one in Robinson et al. (1990). The observation of flare events on old M dwarfs is difficult owing to their infrequency. As such, most flares are caught only as snapshots ...
... of enhanced features, including the Balmer series, during a flare event that we observed which is significantly stronger than the one in Robinson et al. (1990). The observation of flare events on old M dwarfs is difficult owing to their infrequency. As such, most flares are caught only as snapshots ...
Starburst Galaxies - Beck-Shop
... by the arms. The reason why the arms stand out so sharply from the rest of the disk is that they contain numerous star-forming regions. In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in ...
... by the arms. The reason why the arms stand out so sharply from the rest of the disk is that they contain numerous star-forming regions. In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in ...
Variations in Integrated Galactic Initial Mass Functions due to
... Recently, Recchi et al. (2009) investigated the [α/Fe] versus velocity disper142 ...
... Recently, Recchi et al. (2009) investigated the [α/Fe] versus velocity disper142 ...
The Classification of Stellar Spectra
... The early spectral classification system was based on the appearance of the spectra, but the physical reason for these differences in spectra were not understood until the 1930’s and 1940’s. Then it was realized that, while there were some chemical differences among stars, the main thing that determ ...
... The early spectral classification system was based on the appearance of the spectra, but the physical reason for these differences in spectra were not understood until the 1930’s and 1940’s. Then it was realized that, while there were some chemical differences among stars, the main thing that determ ...
Tycho Brahe
... even though he was not the 1st to discover it. (The SNR remnant is visible as a nebula) ...
... even though he was not the 1st to discover it. (The SNR remnant is visible as a nebula) ...
The local ISM in three dimensions: kinematics
... The nearby region of space provides an important test of the theoretical models and simulations since short lines of sight to nearby stars through the local interstellar medium (LISM) should contain fewer velocity structures containing a less diverse range of physical properties than longer lines of ...
... The nearby region of space provides an important test of the theoretical models and simulations since short lines of sight to nearby stars through the local interstellar medium (LISM) should contain fewer velocity structures containing a less diverse range of physical properties than longer lines of ...
A Star - Cloudy Nights
... Double Star Two thirds of all stars in the sky have a companion star. These double stars, or binary star systems have two stars that orbit around a common point. Some double stars orbit each other very quickly (once every few hours), while some orbit each other very slowly (once every few thousand y ...
... Double Star Two thirds of all stars in the sky have a companion star. These double stars, or binary star systems have two stars that orbit around a common point. Some double stars orbit each other very quickly (once every few hours), while some orbit each other very slowly (once every few thousand y ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... the disk rotates; unlike spiral arms, which really are not – they are density waves, rather than physical, distinct physical subsystems, about which we will talk about later. Bars can ...
... the disk rotates; unlike spiral arms, which really are not – they are density waves, rather than physical, distinct physical subsystems, about which we will talk about later. Bars can ...
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.