Variable stars in the globular cluster M 92
... Kadla et al. (1983). They also give the cross-identification of variable stars in the third catalogue of Sawyer-Hogg (1973) with numbering system of Nassau (1938). It appears now that v12 is Nassau’s star no. 10 and v15 corresponds to Nassau’s star no. 12. Oosterhoff (1944) rediscussed the observati ...
... Kadla et al. (1983). They also give the cross-identification of variable stars in the third catalogue of Sawyer-Hogg (1973) with numbering system of Nassau (1938). It appears now that v12 is Nassau’s star no. 10 and v15 corresponds to Nassau’s star no. 12. Oosterhoff (1944) rediscussed the observati ...
ppt - chris.engelbrecht.nithep.ac.za
... calculate the age. How does this compare in the Sedov phase of evolution, ...
... calculate the age. How does this compare in the Sedov phase of evolution, ...
Observational Limits on Terrestrial-Sized Inner Planets Around
... The procedure for instituting the TDA is as follows. First, mutual eclipses of CM Dra are removed from the observed light-curve by the subtraction of a model-eclipse1 . The l i g h t curve is then converted to relative flux values, D(t i) = ∆ F/F o, where the zero-point, F o, i s the average off-ecl ...
... The procedure for instituting the TDA is as follows. First, mutual eclipses of CM Dra are removed from the observed light-curve by the subtraction of a model-eclipse1 . The l i g h t curve is then converted to relative flux values, D(t i) = ∆ F/F o, where the zero-point, F o, i s the average off-ecl ...
Reconciling observations and modelling of thermonuclear bursts
... • Need to compare burst lightcurves as well as energetics and recurrence times at all possible epochs • This has been limited in the past due to the lack of availability of model runs… • … but also the lack of suitable analysis approaches/tools • The pieces are largely in place now to carry out comp ...
... • Need to compare burst lightcurves as well as energetics and recurrence times at all possible epochs • This has been limited in the past due to the lack of availability of model runs… • … but also the lack of suitable analysis approaches/tools • The pieces are largely in place now to carry out comp ...
Article PDF - IOPscience
... target because the data in the other channel were degraded by a scattered light problem in the instrument that has since been resolved. As such, the only filter where all targets observed have data is 692 nm, and this represents our most comprehensive data set. The basic observing strategy has been ...
... target because the data in the other channel were degraded by a scattered light problem in the instrument that has since been resolved. As such, the only filter where all targets observed have data is 692 nm, and this represents our most comprehensive data set. The basic observing strategy has been ...
Evolution of the barium abundance in the early Galaxy from a NLTE
... levels and overpopulates the upper ones (this “pumping” is described e.g. in Bruls et al. 1992, or Asplund 2005). The depth of the effective formation of the radiation in b-b transitions changes significantly with the metallicity (and the corresponding barium abundance) of the star (Fig. 3). This exp ...
... levels and overpopulates the upper ones (this “pumping” is described e.g. in Bruls et al. 1992, or Asplund 2005). The depth of the effective formation of the radiation in b-b transitions changes significantly with the metallicity (and the corresponding barium abundance) of the star (Fig. 3). This exp ...
EVOLUTION OF THE NUCLEAR ACCRETION DISK
... time as the integrated flux in the broad line has decreased. We propose a scenario in which the emission originates in an asymmetric accretion disk around a supermassive black hole, whose source of ionization is getting dimmer, causing the region of maximum emission to come closer to the center (and ...
... time as the integrated flux in the broad line has decreased. We propose a scenario in which the emission originates in an asymmetric accretion disk around a supermassive black hole, whose source of ionization is getting dimmer, causing the region of maximum emission to come closer to the center (and ...
Swanning Around with Chandra Star and Planet Formation in Cygnus OB2 N. Wright
... Planets: Which environments? ...
... Planets: Which environments? ...
1 C. An expanded description of the work being done on the
... The telescope has always been an important tool for scientists, allowing astronomers to observe distant objects. It seems to represent the way in which our perspective of the Universe has changed drastically over the last 400 years, with the rise of science showing us just how insignificant we are. ...
... The telescope has always been an important tool for scientists, allowing astronomers to observe distant objects. It seems to represent the way in which our perspective of the Universe has changed drastically over the last 400 years, with the rise of science showing us just how insignificant we are. ...
X-ray Observations of Cosmic Accelerators Greg Madejski SLAC/KIPAC
... mirrors used in X-ray astronomy: grazing incidence reflection * Can provide large collecting area (mirror) with small detector volume -> reduction of background! * “Standard” version (surface of precisely polished high Z material) good only up to ~ 10 keV HEAO-B (=Einstein) X-ray Observatory (ca. 19 ...
... mirrors used in X-ray astronomy: grazing incidence reflection * Can provide large collecting area (mirror) with small detector volume -> reduction of background! * “Standard” version (surface of precisely polished high Z material) good only up to ~ 10 keV HEAO-B (=Einstein) X-ray Observatory (ca. 19 ...
MHD seismology as a tool to diagnose the coronae of X
... heating of the corona of ξ-Boo. It should be noted that it is a binary K-Dwarf with the magnetized atmosphere and flaring activities. Observations of the decaying long period oscillation of a stellar megaflare by Anfinogentov et al. (2013): In the decay phase of the U-band light curve of a stellar m ...
... heating of the corona of ξ-Boo. It should be noted that it is a binary K-Dwarf with the magnetized atmosphere and flaring activities. Observations of the decaying long period oscillation of a stellar megaflare by Anfinogentov et al. (2013): In the decay phase of the U-band light curve of a stellar m ...
Dai, S - PulsarAstronomy.net
... Neutron Stars through Astrometric Microlensing Sahu, K. C.; Albrow, M.; Anderson, J.; Bond, H. E.; Bond, I.; Brown, T. M.; Casertano, S.; Dominik, M.; Ferguson, H. C.; Fryer, C.; Livio, M.; Mao, S.; Perrott, Y.; Udalski, A.; Yock, P. 2012, American Astronomical Society Meeting Abstracts, 220, #307.0 ...
... Neutron Stars through Astrometric Microlensing Sahu, K. C.; Albrow, M.; Anderson, J.; Bond, H. E.; Bond, I.; Brown, T. M.; Casertano, S.; Dominik, M.; Ferguson, H. C.; Fryer, C.; Livio, M.; Mao, S.; Perrott, Y.; Udalski, A.; Yock, P. 2012, American Astronomical Society Meeting Abstracts, 220, #307.0 ...
Harvesting ALFALFA: Discovering Galaxies in the Pisces
... ALFALFA Team. This work has been supported by NSF grants AST-1211005, AST1637339 and AST-1637271. The Cornell ALFLAFA Team also appreciates support from NSF/AST-1107390 and the Brinson Foundation. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the Nationa ...
... ALFALFA Team. This work has been supported by NSF grants AST-1211005, AST1637339 and AST-1637271. The Cornell ALFLAFA Team also appreciates support from NSF/AST-1107390 and the Brinson Foundation. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the Nationa ...
C, N, O abundances and carbon isotope ratios in evolved stars of
... we neglected NGC 6253 2508 in the analysis. All stars observed in NGC 6253 belong to the red clump of the cluster (see Fig. 2). In this work as well as in other papers of this series (Mikolaitis et al. 2010, 2011a,b), the atlas models with overshooting (Kurucz 1993) and a computing code by Gratton ( ...
... we neglected NGC 6253 2508 in the analysis. All stars observed in NGC 6253 belong to the red clump of the cluster (see Fig. 2). In this work as well as in other papers of this series (Mikolaitis et al. 2010, 2011a,b), the atlas models with overshooting (Kurucz 1993) and a computing code by Gratton ( ...
The Sun as an X-Ray Star. III. Flares
... by several investigations with the XMM-Newton (X-ray Multi-Mirror Mission) and Chandra satellites (e.g., evidence for an inverse Ðrst ionization potential e†ect has been found on the star HR1099 ; Brinkman et al. 2001), the approach presented here does not allow to investigate it properly. What we c ...
... by several investigations with the XMM-Newton (X-ray Multi-Mirror Mission) and Chandra satellites (e.g., evidence for an inverse Ðrst ionization potential e†ect has been found on the star HR1099 ; Brinkman et al. 2001), the approach presented here does not allow to investigate it properly. What we c ...
ExoPlanet News No. 74, November 3rd, 2014 Contents An Electronic Newsletter
... announcements, and jobs & studentships for future editions Remember that past editions of this newsletter, submission templates and other information can be found at the ExoPlanet News website: http://exoplanet.open.ac.uk. Although note that, as previously notified, following a change to the way our ...
... announcements, and jobs & studentships for future editions Remember that past editions of this newsletter, submission templates and other information can be found at the ExoPlanet News website: http://exoplanet.open.ac.uk. Although note that, as previously notified, following a change to the way our ...
A galaxy rapidly forming stars 700 million years after the Big Bang at
... for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is the progenitor of some of the most massive systems in the high-redshift Universe. However, the z 5 7.213 galaxy GN 108036 (ref. 3), also in the GOODS-North field, also has an implied SFR . 100 M[. Although th ...
... for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is the progenitor of some of the most massive systems in the high-redshift Universe. However, the z 5 7.213 galaxy GN 108036 (ref. 3), also in the GOODS-North field, also has an implied SFR . 100 M[. Although th ...
8th International Workshop on Planetary, Solar and Heliospheric
... older missions like Stereo, Voyager, Galileo, Wind or Ulysses are welcome. Studies of terrestrial radio emission data from missions like MMS, Themis, Van Allen Probes, Cluster or Demeter can be another important topic. In addition to space-based observations, new developments in ground-based radio t ...
... older missions like Stereo, Voyager, Galileo, Wind or Ulysses are welcome. Studies of terrestrial radio emission data from missions like MMS, Themis, Van Allen Probes, Cluster or Demeter can be another important topic. In addition to space-based observations, new developments in ground-based radio t ...
The uniqueness of Antarctica for the study of AGB stars
... B. Accurate study of the variations of luminosity (variability) over the wide region of the electromagnetic spectrum including optical and IR. Which kind of observations can be done from the ground ? Surveys through wide field (future) or small area (IRAIT) imaging of interesting stellar systems. ...
... B. Accurate study of the variations of luminosity (variability) over the wide region of the electromagnetic spectrum including optical and IR. Which kind of observations can be done from the ground ? Surveys through wide field (future) or small area (IRAIT) imaging of interesting stellar systems. ...
Evolution of the Mass-to-light Ratio of Galaxies to z~0.25
... average integration times (half spent on-source) ranged between 2 and 6 hours, making these observations for a significant number of objects currently feasible only at Arecibo. ...
... average integration times (half spent on-source) ranged between 2 and 6 hours, making these observations for a significant number of objects currently feasible only at Arecibo. ...
Rotation - Indiana University Astronomy
... Alternative magnetic field indicators: collimated jets and energetic winds – Jets and winds are likely launched from the disk-magnetosphere boundary – Such winds are ubiquitous among low mass (M < 2 Msun) accreting PMS stars – Direct evidence of jets found among accreting stars as massive as M ~ 10 ...
... Alternative magnetic field indicators: collimated jets and energetic winds – Jets and winds are likely launched from the disk-magnetosphere boundary – Such winds are ubiquitous among low mass (M < 2 Msun) accreting PMS stars – Direct evidence of jets found among accreting stars as massive as M ~ 10 ...
(McCullough et al. 2014).
... spatial scanning will enable observations that otherwise would be compromised by pre-exposure saturation of the IR detector that lacks a physical shutter. For a slitless stellar spectrum, one requires a wavelength-dependent flat field, but now we can get what we want directly, in orbit, using a spat ...
... spatial scanning will enable observations that otherwise would be compromised by pre-exposure saturation of the IR detector that lacks a physical shutter. For a slitless stellar spectrum, one requires a wavelength-dependent flat field, but now we can get what we want directly, in orbit, using a spat ...
Five Planets and an Independent Confirmation of
... We have acquired 45 Doppler measurements of HD 30562 over the past ten years. With typical seeing at Lick of 1.′′ 5, the exposure time for SNR of 140 is about 5 minutes on the 3-m Shane telescope or about 30 minutes on the 0.6-m Coudé Auxiliary Telescope (CAT). The observation dates, radial velocit ...
... We have acquired 45 Doppler measurements of HD 30562 over the past ten years. With typical seeing at Lick of 1.′′ 5, the exposure time for SNR of 140 is about 5 minutes on the 3-m Shane telescope or about 30 minutes on the 0.6-m Coudé Auxiliary Telescope (CAT). The observation dates, radial velocit ...
Two extremely luminous WN stars in the Galactic center with
... λ 2.189 μm feature cannot be due to He ii emission from that star. Therefore we chose as our best-fitting model the grid point that lies closest to the intersection point of the contours for the strong He i λ2.06 μm and He i λ2.115 μm lines. The parameters are T ∗ = 25.1 kK and log Rt = 1.48 (large ...
... λ 2.189 μm feature cannot be due to He ii emission from that star. Therefore we chose as our best-fitting model the grid point that lies closest to the intersection point of the contours for the strong He i λ2.06 μm and He i λ2.115 μm lines. The parameters are T ∗ = 25.1 kK and log Rt = 1.48 (large ...
Research Report for 2015/2016
... using AstroBEAR2.0, Protostars and Planets VI 1K058 Hartigan, P. 2013, "NEWFIRM Observations of PDR Boundaries in Massive Star Formation Regions: The Pillars and Walls of Carina", BAAS 221, 25119 Crockett, C., Mahmud, N., Prato, L., Johns-Krull, C., Hartigan, P., Jaffe, D., and Beichman, C., 2011, S ...
... using AstroBEAR2.0, Protostars and Planets VI 1K058 Hartigan, P. 2013, "NEWFIRM Observations of PDR Boundaries in Massive Star Formation Regions: The Pillars and Walls of Carina", BAAS 221, 25119 Crockett, C., Mahmud, N., Prato, L., Johns-Krull, C., Hartigan, P., Jaffe, D., and Beichman, C., 2011, S ...
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.