![Chalmers Un](http://s1.studyres.com/store/data/017883375_1-ce92bf81f6163ea158a35960db1f8e95-300x300.png)
Chalmers Un
... • Since April 2014: Director of the Master’s program in Physics & Astronomy at Chalmers (MPPAS) and of the corresponding Master’s program in Physics at Gothenburg University (N2PHY). • Since 2012: Reviewer of postdoc applications in astrophysics to Nordita, Stockholm. • Since 2012: Member of the LOF ...
... • Since April 2014: Director of the Master’s program in Physics & Astronomy at Chalmers (MPPAS) and of the corresponding Master’s program in Physics at Gothenburg University (N2PHY). • Since 2012: Reviewer of postdoc applications in astrophysics to Nordita, Stockholm. • Since 2012: Member of the LOF ...
ultracam observations of pulsating sdB stars
... interior of a star. Surface displacement may be characterized by spherical harmonic functions: s = so Yl,m(,) l: degree of the spherical harmonic = number of lines of nodes on a spherical surface m: azimuthal number = number of lines of nodes passing through the polar axis n: order of the spherica ...
... interior of a star. Surface displacement may be characterized by spherical harmonic functions: s = so Yl,m(,) l: degree of the spherical harmonic = number of lines of nodes on a spherical surface m: azimuthal number = number of lines of nodes passing through the polar axis n: order of the spherica ...
Subrahmanyan Chandrasekhar
... Then, aged just 14, he began studying for a physics degree at Presidency College, also in Madras. (The city of Madras is now known as Chennai.) In 1929, aged 18, he wrote his first academic paper, The Compton Scattering and the New Statistics. The following year, he graduated with a B.Sc. Honors deg ...
... Then, aged just 14, he began studying for a physics degree at Presidency College, also in Madras. (The city of Madras is now known as Chennai.) In 1929, aged 18, he wrote his first academic paper, The Compton Scattering and the New Statistics. The following year, he graduated with a B.Sc. Honors deg ...
Evolved massive stars in W33 and in GMC G23.3-0.3
... and at the parallactic distance of 2.4 kpc (Immer et al. 2013). We spectroscopically detected a few evolved O-type stars and one Wolf-Rayet star, but none of the late-type objects has the luminosity of a RSG star. Several dense molecular cores that may harbor proto clusters were recently discovered ...
... and at the parallactic distance of 2.4 kpc (Immer et al. 2013). We spectroscopically detected a few evolved O-type stars and one Wolf-Rayet star, but none of the late-type objects has the luminosity of a RSG star. Several dense molecular cores that may harbor proto clusters were recently discovered ...
Formation of Active Regions on the Rising Slope of the 23rd Solar
... Peak National Observatory and Mount Wilson Observatory, also with H-α images and photo-heliograms [2]. For some of the solar activity cycles many authors studied distribution of the active regions at the chromospheric level in relation to the boundaries of large background fields [3-9]. In this work ...
... Peak National Observatory and Mount Wilson Observatory, also with H-α images and photo-heliograms [2]. For some of the solar activity cycles many authors studied distribution of the active regions at the chromospheric level in relation to the boundaries of large background fields [3-9]. In this work ...
Slides
... primarily serves qualitative analyses of sediments (mineral and organic phase) It is also uses for quantitative analyses (iron, clay, OM) Applicable to study analogues ...
... primarily serves qualitative analyses of sediments (mineral and organic phase) It is also uses for quantitative analyses (iron, clay, OM) Applicable to study analogues ...
Lecture 26 Pre-Main Sequence Evolution
... – The class of T Tauri stars was defined after the prototype T Tau • Irregular variability by as much as 3 magnitudes • Spectral types F5 to G5, with strong Ca II H & K emission lines as well as H Balmer lines • Low luminosity • Association with either bright or dark nebulosity • Later extend to all ...
... – The class of T Tauri stars was defined after the prototype T Tau • Irregular variability by as much as 3 magnitudes • Spectral types F5 to G5, with strong Ca II H & K emission lines as well as H Balmer lines • Low luminosity • Association with either bright or dark nebulosity • Later extend to all ...
Third-World Astronomy Network Jayant V. Narlikar Inter
... required. Some NIs may already have an infrastructure for their own needs. But it may have to be upgraded to take on the additional responsibility of the nodal role. Some project staff may have to be appointed for running and maintaining the facility. Since the job market lures the talented to comme ...
... required. Some NIs may already have an infrastructure for their own needs. But it may have to be upgraded to take on the additional responsibility of the nodal role. Some project staff may have to be appointed for running and maintaining the facility. Since the job market lures the talented to comme ...
Spots on Ap Stars
... • Expect polar spots, equatorial rings • Si depleted in polar spots, enhanced in rings • Cr enhanced in polar spots, depleted in rings • Element diffusion along horizontal field lines may cause surface abundance distributions to evolve with time (time ...
... • Expect polar spots, equatorial rings • Si depleted in polar spots, enhanced in rings • Cr enhanced in polar spots, depleted in rings • Element diffusion along horizontal field lines may cause surface abundance distributions to evolve with time (time ...
T Tauri Variable Type Star
... Pre Main Sequence – young, low mass stars that are contracting as they evolve toward their main sequence stage. Mostly made of Hydrogen, some Helium, and some trace elements. Of the trace elements, Lithium appears which is an indicator of stellar youth. Often have large protoplanetary accretion disk ...
... Pre Main Sequence – young, low mass stars that are contracting as they evolve toward their main sequence stage. Mostly made of Hydrogen, some Helium, and some trace elements. Of the trace elements, Lithium appears which is an indicator of stellar youth. Often have large protoplanetary accretion disk ...
The s-process in low metallicity stars - GSI
... cross sections are very small and the resulting s-process abundances are large. This happens at the first s-peak at Sr, Y, Zr, at the second s-peak at Ba, La, Ce, Pr, Nd and eventually at the termination of the s-process involving Pb-208 (and Bi). ...
... cross sections are very small and the resulting s-process abundances are large. This happens at the first s-peak at Sr, Y, Zr, at the second s-peak at Ba, La, Ce, Pr, Nd and eventually at the termination of the s-process involving Pb-208 (and Bi). ...
Types of Telescopes - NSTA Learning Center
... Today, astronomers use digital detectors, such as CCDs (Charged-Coupled Devices): Solid-state semi-conductor chips that use the photoelectric effect. Photons knock electrons loose when they collide with certain elements. Loose electrons create a charge that we measure. ...
... Today, astronomers use digital detectors, such as CCDs (Charged-Coupled Devices): Solid-state semi-conductor chips that use the photoelectric effect. Photons knock electrons loose when they collide with certain elements. Loose electrons create a charge that we measure. ...
PDF Printable and Static Version
... one observational session on the Faulkes telescopes in Hawaii and Australia. We are very grateful to Sarah Roberts, the astronomer from the team of the 2-meter Faulkes telescope project for her help and collaboration. The Director of the National Astronomical Observatory “Rozhen” in Bulgaria will pr ...
... one observational session on the Faulkes telescopes in Hawaii and Australia. We are very grateful to Sarah Roberts, the astronomer from the team of the 2-meter Faulkes telescope project for her help and collaboration. The Director of the National Astronomical Observatory “Rozhen” in Bulgaria will pr ...
The Roles of Small Telescopes in a Virtual Observatory Environment
... Moreover, the universe itself imposes selection effects on what can be seen at any given wavelength: for example, obscuration by dust can hide bursts of star formation and active galactic nuclei from the view in the visible or UV light. ...
... Moreover, the universe itself imposes selection effects on what can be seen at any given wavelength: for example, obscuration by dust can hide bursts of star formation and active galactic nuclei from the view in the visible or UV light. ...
lec1_2008 - Stanford Solar Physics
... all along the sidereal year. The value of this angle is near zero around Earth perihelion and aphelion. The distance of the Sun’s rotational poles from the limb has been exaggerated: at maximum the shift reaches 7°. We can only see the sunspots’ paths as straight lines in early June and December. ...
... all along the sidereal year. The value of this angle is near zero around Earth perihelion and aphelion. The distance of the Sun’s rotational poles from the limb has been exaggerated: at maximum the shift reaches 7°. We can only see the sunspots’ paths as straight lines in early June and December. ...
L173 HAT-P-5b: A JUPITER-LIKE HOT JUPITER TRANSITING A
... addition of new discoveries is valuable. Over the past year the HATNet project11 (Bakos et al. 2002, 2004), a wide-angle photometric survey, has announced four TEPs. In this Letter we report on the detection of a new transiting exoplanet, which we label HAT-P-5b, and our determination of its paramet ...
... addition of new discoveries is valuable. Over the past year the HATNet project11 (Bakos et al. 2002, 2004), a wide-angle photometric survey, has announced four TEPs. In this Letter we report on the detection of a new transiting exoplanet, which we label HAT-P-5b, and our determination of its paramet ...
AAS_WFXT_Solar_System_11Jan2010
... ACIS-S Lunar nightside emission, Wargelin et al. 2004 (see also Wargelin et al. 2009 Chandra posters @ this meeting) ...
... ACIS-S Lunar nightside emission, Wargelin et al. 2004 (see also Wargelin et al. 2009 Chandra posters @ this meeting) ...
Astrophysics for the next decade
... • Observing the warm cores of molecular clouds – Important: spatial resolution and large wavelength coverage – IR observations with large (>8m) telescopes, CanariCam (GTC), VLTI (MATISSE) JWST, ELTs – ALMA will be the champion for this field Wolf & Klahr 2005 ...
... • Observing the warm cores of molecular clouds – Important: spatial resolution and large wavelength coverage – IR observations with large (>8m) telescopes, CanariCam (GTC), VLTI (MATISSE) JWST, ELTs – ALMA will be the champion for this field Wolf & Klahr 2005 ...
Rotational spin-up in the 30-Myr
... 11. Constraints for scheduling observations for this application: Idealy the observations should be scheduled directly after the Chilean time, and should consist of 2hr blocks observed over 15 consecutive nights. 12. Observational experience of observer(s) named under 2.3: (at least one observer mus ...
... 11. Constraints for scheduling observations for this application: Idealy the observations should be scheduled directly after the Chilean time, and should consist of 2hr blocks observed over 15 consecutive nights. 12. Observational experience of observer(s) named under 2.3: (at least one observer mus ...
ppt
... Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
... Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
Naming the 2008-2009 Minimum and Responding to Temperature Declines
... There would be significant areas of the world frozen then. And some of the world’s oceans would freeze as well with unclear effects. I have seen the Seine River in Paris during a rare 2003 snowstorm. There was some talk of a flood risk while there. With severe decreases in temperature related to sol ...
... There would be significant areas of the world frozen then. And some of the world’s oceans would freeze as well with unclear effects. I have seen the Seine River in Paris during a rare 2003 snowstorm. There was some talk of a flood risk while there. With severe decreases in temperature related to sol ...
observational requirements, feasability, expectations
... Need for a precise correction of very low frequency instrumental noise!! Good to have ground observations to have Ca H & K measurements (Mt Wilson index) ...
... Need for a precise correction of very low frequency instrumental noise!! Good to have ground observations to have Ca H & K measurements (Mt Wilson index) ...
NASA Budget Update - Paul Hertz
... Includes $50M for continued preformulation of WFIRST, an increase of $36M over the Administration request and comparable to FY14 Includes $70M for continued SOFIA operations, a reduction of $14M (17%) from FY14 Directs NASA to (a) seek partners to restore SOFIA to its full level, and (b) not t ...
... Includes $50M for continued preformulation of WFIRST, an increase of $36M over the Administration request and comparable to FY14 Includes $70M for continued SOFIA operations, a reduction of $14M (17%) from FY14 Directs NASA to (a) seek partners to restore SOFIA to its full level, and (b) not t ...
causes of solar activity - The National Academies of Sciences
... cycles, flares, prominences, and stellar winds. Recent studies suggest that many of these processes are governed by universal laws applicable to both the Sun and other stars[1, 2]. This solar-stellar connection can be used to extend our understanding of stellar phenomena via the study of solar proce ...
... cycles, flares, prominences, and stellar winds. Recent studies suggest that many of these processes are governed by universal laws applicable to both the Sun and other stars[1, 2]. This solar-stellar connection can be used to extend our understanding of stellar phenomena via the study of solar proce ...
Indian Institute of Astrophysics
![](https://en.wikipedia.org/wiki/Special:FilePath/IIA_logo.png?width=300)
The Indian Institute of Astrophysics (IIA), with its headquarters in Bangalore (Karnataka state), India, is a premier national institute of India for the study of and research into topics pertaining to astronomy, astrophysics and related subjects.The Institute has a network of laboratories and observatories located in various places in India, including Kodaikanal (the Kodaikanal Solar Observatory), Kavalur (the Vainu Bappu Observatory), Gauribidanur, Hanle (the Indian Astronomical Observatory) and Hosakote.