CoRoT Observations of O Stars: Diverse Origins of Variability
... show that all 300 frequencies are significant. It is, however, highly suspicious that so many pulsation frequencies would be present in a single star. The time-frequency diagram (Fig. 1, right) clearly shows that none of these frequencies are stable. They are therefore not pulsational frequencies. A ...
... show that all 300 frequencies are significant. It is, however, highly suspicious that so many pulsation frequencies would be present in a single star. The time-frequency diagram (Fig. 1, right) clearly shows that none of these frequencies are stable. They are therefore not pulsational frequencies. A ...
Astronomy
... 1. Early astronomers identified celestial objects with _________ and ___________. 2. List five phenomena that early astronomers linked to celestial changes. ...
... 1. Early astronomers identified celestial objects with _________ and ___________. 2. List five phenomena that early astronomers linked to celestial changes. ...
Precision UBVJH Single Channel Photometry of Epsilon Aurigae
... Fritsch in 1821, this system has been observed in detail through most of the eclipses since. A concentrated effort was put forth during the 1982 1984 eclipse. While much was learned, many questions still went unanswered. Most astronomers interested in epsilon Aurigae tend to only get excited about i ...
... Fritsch in 1821, this system has been observed in detail through most of the eclipses since. A concentrated effort was put forth during the 1982 1984 eclipse. While much was learned, many questions still went unanswered. Most astronomers interested in epsilon Aurigae tend to only get excited about i ...
ppt - Stratospheric Observatory for Infrared Astronomy
... • Occultation studies with SOFIA will probe the sizes, atmospheres, and possible satellites of newly discovered planet-like objects in the outer Solar system. • The unique mobility of SOFIA opens up some hundred events per year for study compared to a handful for fixed observatories. ...
... • Occultation studies with SOFIA will probe the sizes, atmospheres, and possible satellites of newly discovered planet-like objects in the outer Solar system. • The unique mobility of SOFIA opens up some hundred events per year for study compared to a handful for fixed observatories. ...
Debris Belts Around Vega
... sky, so we’re looking at one of its poles, and its debris disk is seen face-on, not edge on. We can’t detect planets by the “transit” method since they wouldn’t pass in front of the star from our perspective. We can’t detect planets by the “Doppler” method because stars like Vega rotate very fast an ...
... sky, so we’re looking at one of its poles, and its debris disk is seen face-on, not edge on. We can’t detect planets by the “transit” method since they wouldn’t pass in front of the star from our perspective. We can’t detect planets by the “Doppler” method because stars like Vega rotate very fast an ...
HKU Seminar schedule draft
... 08:45 – 10:45 Continuation of Working sessions along the three thematic lines 11:15 – 13:15 Exchange between the three working groups 13:30 Departure by bus towards the Tenerife Telescope area. On the way: Lunch in El Portillo – just 10 minutes from the Observatory. Visit of the Observatory guided b ...
... 08:45 – 10:45 Continuation of Working sessions along the three thematic lines 11:15 – 13:15 Exchange between the three working groups 13:30 Departure by bus towards the Tenerife Telescope area. On the way: Lunch in El Portillo – just 10 minutes from the Observatory. Visit of the Observatory guided b ...
Exoplanet Reflections: the light from 51 Peg b
... where Ag represents the planetary geometrical albedo (several albedo definitions exist (e.g. Marley et al. 1999; Collier Cameron et al. 2002; Seager 2010), but we will here only consider the geometric albedo Ag , defined as the ratio of a planet’s flux measured at opposition (α = 0) by the flux of a ...
... where Ag represents the planetary geometrical albedo (several albedo definitions exist (e.g. Marley et al. 1999; Collier Cameron et al. 2002; Seager 2010), but we will here only consider the geometric albedo Ag , defined as the ratio of a planet’s flux measured at opposition (α = 0) by the flux of a ...
ATNF Steering Committee – Astrophysics highlights
... techniques. It consists of 4300 galaxies, and constitutes the largest blind HI survey by well over an order of magnitude. Reliability and completion have been thoroughly analysed through simulation and reobservation and release of this catalogue will be a valuable resource to the astronomical commun ...
... techniques. It consists of 4300 galaxies, and constitutes the largest blind HI survey by well over an order of magnitude. Reliability and completion have been thoroughly analysed through simulation and reobservation and release of this catalogue will be a valuable resource to the astronomical commun ...
New Discoveries in Planetary Systems and Star Formation through
... the areas of planet and star formation. Studies from the radio to X-rays contribute to our overall understanding of the physical and chemical processes. Understanding the process of accretion is key to astrophysics from the formation of the lowest mass stars to the growth of super-massive black hol ...
... the areas of planet and star formation. Studies from the radio to X-rays contribute to our overall understanding of the physical and chemical processes. Understanding the process of accretion is key to astrophysics from the formation of the lowest mass stars to the growth of super-massive black hol ...
Hot Stars With Cool Companions
... evolution of any planets, and so a census of the multiplicity properties of nearby intermediate mass stars is needed. Additionally, the multiplicity can help constrain the important binary star formation physics. We report initial results from a spectroscopic survey of 400 nearby A- and B-type stars ...
... evolution of any planets, and so a census of the multiplicity properties of nearby intermediate mass stars is needed. Additionally, the multiplicity can help constrain the important binary star formation physics. We report initial results from a spectroscopic survey of 400 nearby A- and B-type stars ...
M - IMAG2E
... • M and R can be measured directly in small numbers of stars (will cover more of this later) • Age and chemical composition also dictate the position of stars in the HR diagram • Stellar clusters very useful laboratories – all stars at same distance, same t, and initial Z • We will develop models to ...
... • M and R can be measured directly in small numbers of stars (will cover more of this later) • Age and chemical composition also dictate the position of stars in the HR diagram • Stellar clusters very useful laboratories – all stars at same distance, same t, and initial Z • We will develop models to ...
scientific paper
... Fitting the orbit of a solar system satellite requires correctly accounting for the changing viewing geometry due to the motion of Earth and the primary in addition to the orbit of the satellite. With a limited number of observations, the orbital solutions can be plagued by aliases of different orbi ...
... Fitting the orbit of a solar system satellite requires correctly accounting for the changing viewing geometry due to the motion of Earth and the primary in addition to the orbit of the satellite. With a limited number of observations, the orbital solutions can be plagued by aliases of different orbi ...
Curriculum Vitae
... Postgraduate level 19 Yrs. Undergraduate level 21 Yrs. Taught the following courses: Thermodynamics and Statistical Physics, Optics and Classical Mechanics, Nuclear Physics, Electricity and Electronics, Quantum Mechanics and Spectroscopy, Classical Electrodynamics, Advanced Quantum Mechanics, Microw ...
... Postgraduate level 19 Yrs. Undergraduate level 21 Yrs. Taught the following courses: Thermodynamics and Statistical Physics, Optics and Classical Mechanics, Nuclear Physics, Electricity and Electronics, Quantum Mechanics and Spectroscopy, Classical Electrodynamics, Advanced Quantum Mechanics, Microw ...
14 September/October 2006 - Tauranga Astronomical Society
... attracted a substantial crowd – standing room only – and was very well received. Dr Christie earned fame last year, (and was awarded the New Zealand Order of Merit) for his part in taking observations contributing to the discovery of an Earth sized planet beyond our solar system. He has been involve ...
... attracted a substantial crowd – standing room only – and was very well received. Dr Christie earned fame last year, (and was awarded the New Zealand Order of Merit) for his part in taking observations contributing to the discovery of an Earth sized planet beyond our solar system. He has been involve ...
High-Resolution Spectroscopy of the Transiting Planet Host Star
... excitation potentials 0.86 ≤ x l ≤ 5.03 eV and 2.58 ≤ x l ≤ 3.90 eV, respectively) from the HIRES spectrum and used standard packages in IRAF to derive equivalent widths (EWs) for all of them. Our selection of lines and transition probabilities followed that of Lee & Carney (2002). ...
... excitation potentials 0.86 ≤ x l ≤ 5.03 eV and 2.58 ≤ x l ≤ 3.90 eV, respectively) from the HIRES spectrum and used standard packages in IRAF to derive equivalent widths (EWs) for all of them. Our selection of lines and transition probabilities followed that of Lee & Carney (2002). ...
Cepheid variable stars
... more than 2400 variable stars. Looking at the variable stars that she had discovered in the Small Magellanic Cloud, Leavitt noticed that Cepheids with long pulsation periods were intrinsically more luminous than their short period counterparts. Her discovery was the basis of the Cepheid period-lumin ...
... more than 2400 variable stars. Looking at the variable stars that she had discovered in the Small Magellanic Cloud, Leavitt noticed that Cepheids with long pulsation periods were intrinsically more luminous than their short period counterparts. Her discovery was the basis of the Cepheid period-lumin ...
Презентация PowerPoint - INSTITUTE OF ASTRONOMY
... Comparing the LSST (8.4 m) telescope with the SDSS, and allowing also for its increased pixel sampling and resolution, the advantage in figure of merit is by a factor of close to 200 Data products will consist of photometric catalogs which will be continuously updating during the survey, a moving ob ...
... Comparing the LSST (8.4 m) telescope with the SDSS, and allowing also for its increased pixel sampling and resolution, the advantage in figure of merit is by a factor of close to 200 Data products will consist of photometric catalogs which will be continuously updating during the survey, a moving ob ...
http://www.lanl.gov/orgs/adtsc/publications/science_highlights_2013/docs/Pg24_25.pdf
... To learn more about 2012aw and to test the physical accuracy of our new simulation pipeline, we ran a series of simulations and compared their lightcurves to 2012aw. We began with a previously run 2-Msun progenitor that showed similar lightcurve characteristics and modified the wind profile to obtai ...
... To learn more about 2012aw and to test the physical accuracy of our new simulation pipeline, we ran a series of simulations and compared their lightcurves to 2012aw. We began with a previously run 2-Msun progenitor that showed similar lightcurve characteristics and modified the wind profile to obtai ...
Revised physical elements of the astrophysically important O9.5+O9
... Aims. Thanks to its long and rich observational history and rapid apsidal motion, the massive eclipsing binary Y Cyg represents one of the cornerstones of critical tests of stellar evolutionary theory for massive stars. Nevertheless, the determination of the basic physical properties is less accurat ...
... Aims. Thanks to its long and rich observational history and rapid apsidal motion, the massive eclipsing binary Y Cyg represents one of the cornerstones of critical tests of stellar evolutionary theory for massive stars. Nevertheless, the determination of the basic physical properties is less accurat ...
Ground-Based Astronomy in Belgium. ESO and the E-ELT.
... What ESA is for astronomy from space (and CERN is for particle physics), ESO is for ground-based astronomy. However, the specific industrial boundary conditions (contract placement, geo-return policy …) in the two different organizations differ. The scientific communities exploiting ESO in Belgium a ...
... What ESA is for astronomy from space (and CERN is for particle physics), ESO is for ground-based astronomy. However, the specific industrial boundary conditions (contract placement, geo-return policy …) in the two different organizations differ. The scientific communities exploiting ESO in Belgium a ...
The edge of the solar system - Beck-Shop
... be discovered. He called this distant object ‘Planet X’ and, like Pickering, he tried to calculate where in the sky it might be found. However, Lowell had an advantage over his rival, for he had the means to pursue his search without relying on the whims of others. Lowell owned a private observatory ...
... be discovered. He called this distant object ‘Planet X’ and, like Pickering, he tried to calculate where in the sky it might be found. However, Lowell had an advantage over his rival, for he had the means to pursue his search without relying on the whims of others. Lowell owned a private observatory ...
ph507lecnote07
... Photograph of the solar corona during the July, 1991 eclipse, at the peak of the sunspot cycle. At these times, the corona is much less regular and much more extended than at sunspot minimum. Astronomers believe that coronal heating is caused by surface activity on the Sun. The changing shape and si ...
... Photograph of the solar corona during the July, 1991 eclipse, at the peak of the sunspot cycle. At these times, the corona is much less regular and much more extended than at sunspot minimum. Astronomers believe that coronal heating is caused by surface activity on the Sun. The changing shape and si ...
Document
... But some gases escape and cannot be determined this way (for example hydrogen, or noble gases) Not all meteorites are suitable - most of them are fractionated and do not provide representative solar abundance information. One needs primitive meteorites that underwent little modification after ...
... But some gases escape and cannot be determined this way (for example hydrogen, or noble gases) Not all meteorites are suitable - most of them are fractionated and do not provide representative solar abundance information. One needs primitive meteorites that underwent little modification after ...
Article PDF - IOPscience
... orbit, this would limit the length of an eclipse in such a system to ≤7 days, much shorter than observed. In addition, we note that there is no evidence of a second source of light in the system, as might be expected if the unseen feature were more massive than the K7 star. Therefore, we expect that ...
... orbit, this would limit the length of an eclipse in such a system to ≤7 days, much shorter than observed. In addition, we note that there is no evidence of a second source of light in the system, as might be expected if the unseen feature were more massive than the K7 star. Therefore, we expect that ...
Transparencies - Rencontres de Moriond
... More photons from the larger collecting area ( fainter sources within reach, higher S/N ratios for brightest sources) For photon-noise dominated observations, the S/N gain proportional to D at fixed time and flux, the speed (1/ time required to reach given S/N ) to D2 ). For sky limited observat ...
... More photons from the larger collecting area ( fainter sources within reach, higher S/N ratios for brightest sources) For photon-noise dominated observations, the S/N gain proportional to D at fixed time and flux, the speed (1/ time required to reach given S/N ) to D2 ). For sky limited observat ...
Indian Institute of Astrophysics
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.