azu_etd_13224_sip1_m
... wanted during this time. I was also supported during the summer by Dr. Griffith’s NASA’s Planetary Atmospheres Program grant, and during this last year by a NASA Keck PI grant. In addition, my thesis was possible due to the data available in the Keck Observatory Archive (KOA), operated by the W. M. ...
... wanted during this time. I was also supported during the summer by Dr. Griffith’s NASA’s Planetary Atmospheres Program grant, and during this last year by a NASA Keck PI grant. In addition, my thesis was possible due to the data available in the Keck Observatory Archive (KOA), operated by the W. M. ...
THE DAWN OF X-RAY ASTRONOMY
... to identify binary x-ray sources, supernovas, galaxies, active galaxies, quasars, and clusters of galaxies (Fig. 4). But even more important from a certain point of view was the ability, which was provided by the control system, to slow down the satellite spin and spend a very long time on an indivi ...
... to identify binary x-ray sources, supernovas, galaxies, active galaxies, quasars, and clusters of galaxies (Fig. 4). But even more important from a certain point of view was the ability, which was provided by the control system, to slow down the satellite spin and spend a very long time on an indivi ...
PhD thesis - Hamburger Sternwarte
... to take into account the properties of the HRT spectrograph. The data reduction pipeline was designed to automatically perform all standard reduction steps for Échelle spectra including an automatic wavelength calibration. During the observations form Oct. 2008 until Aug. 2009, the pipeline was sho ...
... to take into account the properties of the HRT spectrograph. The data reduction pipeline was designed to automatically perform all standard reduction steps for Échelle spectra including an automatic wavelength calibration. During the observations form Oct. 2008 until Aug. 2009, the pipeline was sho ...
The Very precise Echelle SpectroPolarimeter on the Araki telescope
... distributions and velocity fields of the circumstellar environment of these stars. Given that the degree of polarization of the light from the stars is typically 1% or less, the polarimetric accuracy must be less than δP = 0.1% for linear polarization to detect polarization variations via changes in ...
... distributions and velocity fields of the circumstellar environment of these stars. Given that the degree of polarization of the light from the stars is typically 1% or less, the polarimetric accuracy must be less than δP = 0.1% for linear polarization to detect polarization variations via changes in ...
Full Programme and Abstracts - UK Exoplanet community meeting
... of the core to the rise of atmospheric oxygen. This detailed understanding can benefit our perspective of exo-planetary systems, whilst at the same time deepening our knowledge of Earth’s formation. Profound questions still remain as to the origin of Earth’s atmosphere, continents, and habitable cli ...
... of the core to the rise of atmospheric oxygen. This detailed understanding can benefit our perspective of exo-planetary systems, whilst at the same time deepening our knowledge of Earth’s formation. Profound questions still remain as to the origin of Earth’s atmosphere, continents, and habitable cli ...
Galaxies
... 72. Until recently, most astronomers thought elliptical galaxies were shaped like oblate spheroids. ...
... 72. Until recently, most astronomers thought elliptical galaxies were shaped like oblate spheroids. ...
- Spiral - Imperial College London
... direct and inverse correlations of visible irradiance (e.g. as measured in the Strömgren b and y filters) and activity, that there is evidence for both the direct (e.g. Lean et al. 2005; Krivova & Solanki 2008; Krivova et al. 2010; Ball et al. 2011) and inverse (Harder et al. 2009; Preminger et al. ...
... direct and inverse correlations of visible irradiance (e.g. as measured in the Strömgren b and y filters) and activity, that there is evidence for both the direct (e.g. Lean et al. 2005; Krivova & Solanki 2008; Krivova et al. 2010; Ball et al. 2011) and inverse (Harder et al. 2009; Preminger et al. ...
Analysis of Stellar Activity and Orbital Dynamics in Extrasolar
... the terrestrial planets to accrete waterrich material from the Main Asteroid Belt, which could explain the existence of water on the terrestrial planets today (O’Brien et al., 2006). In its T Tauri phase the protosun accretes matter from the surrounding protoplanetary disk and contracts until the co ...
... the terrestrial planets to accrete waterrich material from the Main Asteroid Belt, which could explain the existence of water on the terrestrial planets today (O’Brien et al., 2006). In its T Tauri phase the protosun accretes matter from the surrounding protoplanetary disk and contracts until the co ...
The following is a supplemental addendum to the included
... each axis has an equal amount of travel to move in either direction. Once the index position has been set, the hand control will display the last entered date and time information stored in the hand control. Once the telescope is powered on: 1. Press ENTER begin the alignment process. 2. Press ENTER ...
... each axis has an equal amount of travel to move in either direction. Once the index position has been set, the hand control will display the last entered date and time information stored in the hand control. Once the telescope is powered on: 1. Press ENTER begin the alignment process. 2. Press ENTER ...
The Alpha Centauri binary system
... α Cen A, and Teff = 5240 K, [Fe/H] = +0.25, log g = 4.44 and ξt = 1.28 km s−1 for α Cen B. The parameters were derived from the simultaneous excitation & ionization equilibria of the equivalent widths of Fe I and Fe II lines. Effective temperatures were also obtained by fitting theoretical profiles ...
... α Cen A, and Teff = 5240 K, [Fe/H] = +0.25, log g = 4.44 and ξt = 1.28 km s−1 for α Cen B. The parameters were derived from the simultaneous excitation & ionization equilibria of the equivalent widths of Fe I and Fe II lines. Effective temperatures were also obtained by fitting theoretical profiles ...
The Perseid Meteor Shower
... Swift-Tuttle. It is named after two American scientists who discovered the comet in 1862. The scientists were not working together. They were each looking through their own telescopes and saw the comet. Lewis Swift saw it first and then, three days later, Horace Tuttle saw it. As the comet got close ...
... Swift-Tuttle. It is named after two American scientists who discovered the comet in 1862. The scientists were not working together. They were each looking through their own telescopes and saw the comet. Lewis Swift saw it first and then, three days later, Horace Tuttle saw it. As the comet got close ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... 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 simple pair of binoculars, and that you know nothing of astronomy or the ...
... 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 simple pair of binoculars, and that you know nothing of astronomy or the ...
pdf of talks and poster abstracts
... complementing Gaia beyond its limit of sensitivity and down the planetary mass domain. Using ground based observations, we derive proper motions with an accuracy as good as 0.3mas/yr up to i=23~24mag. These accurate measurements allow us to identify the members, and study the properties of the clust ...
... complementing Gaia beyond its limit of sensitivity and down the planetary mass domain. Using ground based observations, we derive proper motions with an accuracy as good as 0.3mas/yr up to i=23~24mag. These accurate measurements allow us to identify the members, and study the properties of the clust ...
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 ...
Follow Proxima Centauri - Department of Physics and Astronomy
... A parsec is 3.26 light years, and Proxima Centauri is 1.3 parsecs. If we could watch it appear to move during the year, it would follow a little ellipse in the sky about 1/1.3 arcseconds in semimajor axis, that is about 2/1.3 arcseconds across. As you will see soon, this is a very very small angle. ...
... A parsec is 3.26 light years, and Proxima Centauri is 1.3 parsecs. If we could watch it appear to move during the year, it would follow a little ellipse in the sky about 1/1.3 arcseconds in semimajor axis, that is about 2/1.3 arcseconds across. As you will see soon, this is a very very small angle. ...
AAVSO: Epsilon Aurigae
... Will the shape of the light curve in different wavelengths change relative to the 1984-85 eclipse, indicating precession or other physical changes in the inner region of the eclipsing disk? There's a lot left to study in this star, and a lot of time between now and the eclipse to observe. The eclips ...
... Will the shape of the light curve in different wavelengths change relative to the 1984-85 eclipse, indicating precession or other physical changes in the inner region of the eclipsing disk? There's a lot left to study in this star, and a lot of time between now and the eclipse to observe. The eclips ...
Evolution of stars
... a. are spectral type M stars. b. are spectral type O stars. c. are located at the bottom of the main sequence in the HR diagram. d. have masses very similar to the sun. e. both b and c The star Algol is a. an astrometric binary. b. a single line spectroscopic binary. c. a visual binary. d. an eclips ...
... a. are spectral type M stars. b. are spectral type O stars. c. are located at the bottom of the main sequence in the HR diagram. d. have masses very similar to the sun. e. both b and c The star Algol is a. an astrometric binary. b. a single line spectroscopic binary. c. a visual binary. d. an eclips ...
Galileo`s miraculous year: 1609 and the revolutionary telescope
... recognise that the star diameters he measured were due to diffraction through the collimators of his lenses (and other effects), not the true magnified star diameters. Over the years, the two stars of Mizar did not show any parallax that Galileo could observe. Of course no such parallax of Mizar, tru ...
... recognise that the star diameters he measured were due to diffraction through the collimators of his lenses (and other effects), not the true magnified star diameters. Over the years, the two stars of Mizar did not show any parallax that Galileo could observe. Of course no such parallax of Mizar, tru ...
Galileo`s Observation of Neptune 1612-1613
... Just about all of the “fixed stars” Galileo records in his notebooks while observing Jupiter appear in modern star catalogues. However one of those “fixed stars”, seen in December 1612 and January 1613 does not appear in any star catalogue. This particular “fixed star” turns out to be something enti ...
... Just about all of the “fixed stars” Galileo records in his notebooks while observing Jupiter appear in modern star catalogues. However one of those “fixed stars”, seen in December 1612 and January 1613 does not appear in any star catalogue. This particular “fixed star” turns out to be something enti ...
disappearance of comet c/2010 x1 (elenin): gone with a whimper
... each spacecraft, HI is equipped with two cameras, HI-1 and HI2, having small (20°) and large (70n) angular fields of view, respectively. The camera centers point away from the Sun by 14°(HI-1) and 53◦. 7 (HI-2). The spectral passbands of the HI-1 cameras cover wavelengths from 630 to 730 nm, similar ...
... each spacecraft, HI is equipped with two cameras, HI-1 and HI2, having small (20°) and large (70n) angular fields of view, respectively. The camera centers point away from the Sun by 14°(HI-1) and 53◦. 7 (HI-2). The spectral passbands of the HI-1 cameras cover wavelengths from 630 to 730 nm, similar ...
21 -26 August University of Exeter
... The past few years have seen a great deal of spectacular large-scale surveys of star-forming regions across the Galaxy with unprecedented sensitivity and angular resolution. Combined with state-of-the-art interferometric follow-up observations, these surveys are transforming our view and understandi ...
... The past few years have seen a great deal of spectacular large-scale surveys of star-forming regions across the Galaxy with unprecedented sensitivity and angular resolution. Combined with state-of-the-art interferometric follow-up observations, these surveys are transforming our view and understandi ...
Why is the Sun very dense on the inside?
... a) Some stars are larger than others and therefore appear larger. b) Some stars are nearer than others and therefore appear larger. c) Photographs make brighter stars appear larger than fainter stars, although they should all be points of light. d) Sometimes what looks like a single star is actu ...
... a) Some stars are larger than others and therefore appear larger. b) Some stars are nearer than others and therefore appear larger. c) Photographs make brighter stars appear larger than fainter stars, although they should all be points of light. d) Sometimes what looks like a single star is actu ...
Hipparcos
Hipparcos was a scientific satellite of the European Space Agency (ESA), launched in 1989 and operated until 1993. It was the first space experiment devoted to precision astrometry, the accurate measurement of the positions of celestial objects on the sky. This permitted the accurate determination of proper motions and parallaxes of stars, allowing a determination of their distance and tangential velocity. When combined with radial-velocity measurements from spectroscopy, this pinpointed all six quantities needed to determine the motion of stars. The resulting Hipparcos Catalogue, a high-precision catalogue of more than 118,200 stars, was published in 1997. The lower-precision Tycho Catalogue of more than a million stars was published at the same time, while the enhanced Tycho-2 Catalogue of 2.5 million stars was published in 2000. Hipparcos ' follow-up mission, Gaia, was launched in 2013.The word ""Hipparcos"" is an acronym for High precision parallax collecting satellite and also a reference to the ancient Greek astronomer Hipparchus of Nicaea, who is noted for applications of trigonometry to astronomy and his discovery of the precession of the equinoxes.