SDSS J105754. 25+ 275947.5: a period
... Car. However, as stated in McAllister et al. (2015), we feel this is still a reasonable assumption to make due to agreement between photometric and spectroscopic parameter estimates (Copperwheat et al. 2012; Savoury et al. 2012). Due to the tenuous bright spot in SDSS 1057, a simple bright spot mode ...
... Car. However, as stated in McAllister et al. (2015), we feel this is still a reasonable assumption to make due to agreement between photometric and spectroscopic parameter estimates (Copperwheat et al. 2012; Savoury et al. 2012). Due to the tenuous bright spot in SDSS 1057, a simple bright spot mode ...
paper - Harvard-Smithsonian Center for Astrophysics
... These findings justify the need to consider a non-LTE radiative transfer model to interpret the measured fluxes. We perform this analysis using the RADEX package (van der Tak et al. 2007), which calculates expected line intensities for a given column density of SO2 , kinetic temperature (Tkin ), and ...
... These findings justify the need to consider a non-LTE radiative transfer model to interpret the measured fluxes. We perform this analysis using the RADEX package (van der Tak et al. 2007), which calculates expected line intensities for a given column density of SO2 , kinetic temperature (Tkin ), and ...
Philosophy of Graduate Education at Rochester
... Departments at Rochester are about Half the Size of Departments at larger universities. Individually we are small, collectively we are large and diverse Individually large departments usually fragment into subfields which rarely communicate with each other ...
... Departments at Rochester are about Half the Size of Departments at larger universities. Individually we are small, collectively we are large and diverse Individually large departments usually fragment into subfields which rarely communicate with each other ...
1 Introduction
... Spectroscopy is the high-frequency analogue of the measurement of spectral lines in the radio astronomy bands below 275 GHz. The wealth of spectral lines throughout the frequency range between 10 THz and 1 000 THz, the vast majority of which are from various states of elements and molecules which do ...
... Spectroscopy is the high-frequency analogue of the measurement of spectral lines in the radio astronomy bands below 275 GHz. The wealth of spectral lines throughout the frequency range between 10 THz and 1 000 THz, the vast majority of which are from various states of elements and molecules which do ...
Chandra News The Secret X-ray Lives of Planetary Nebulae
... less elliptical) central bubble. This object is one of only three diffuse X-ray PNe detected thus far that are seen to depart from a classical “hot bubble’’ morphology: the linear bubble structure that lends the Ant Nebula (Menzel 3) its name appears to be threaded from within by X-ray-emitting jets ...
... less elliptical) central bubble. This object is one of only three diffuse X-ray PNe detected thus far that are seen to depart from a classical “hot bubble’’ morphology: the linear bubble structure that lends the Ant Nebula (Menzel 3) its name appears to be threaded from within by X-ray-emitting jets ...
Variable Star Section Circular - Number 75
... sets at about U h GMAT so only a segment of the fade will be visible. However, any observations obtained from Europe will be very useful as they will complement those from America, where only part of the rise should be visible. Visual observations are made difficult by the lack of suitable compariso ...
... sets at about U h GMAT so only a segment of the fade will be visible. However, any observations obtained from Europe will be very useful as they will complement those from America, where only part of the rise should be visible. Visual observations are made difficult by the lack of suitable compariso ...
chemical abundances for a-and f-type supergiant stars
... The process of chemical evolution in the Galaxy can be understood from the study of its massive stars. These objects in their rapid evolution undergo changes through the process of nucleosynthesis and return their chemical elements to the interstellar medium by stellar winds and supernova events. Th ...
... The process of chemical evolution in the Galaxy can be understood from the study of its massive stars. These objects in their rapid evolution undergo changes through the process of nucleosynthesis and return their chemical elements to the interstellar medium by stellar winds and supernova events. Th ...
Properties and nature of Be stars: 27. Orbital and recent long
... nificant RV changes. Ballereau et al. (1988) carried out an analysis of a homogeneous series of Haute Provence high-dispersion photographic spectra from 1978-1987 and once more concluded that the shell RVs vary with periods of 136.0 and 106.7 days. Katahira et al. (1996a,b) analyzed shell RVs from t ...
... nificant RV changes. Ballereau et al. (1988) carried out an analysis of a homogeneous series of Haute Provence high-dispersion photographic spectra from 1978-1987 and once more concluded that the shell RVs vary with periods of 136.0 and 106.7 days. Katahira et al. (1996a,b) analyzed shell RVs from t ...
THE ORION NEBULA AND ITS ASSOCIATED POPULATION C. R. O
... to have produced three regions of massive star formation, the most luminous of which has produced M 42, but also nearby are imbedded groupings to the NW and SW of the tight clustering of early type stars known as the Trapezium. The historical interest in this region continues through the present, wi ...
... to have produced three regions of massive star formation, the most luminous of which has produced M 42, but also nearby are imbedded groupings to the NW and SW of the tight clustering of early type stars known as the Trapezium. The historical interest in this region continues through the present, wi ...
Jaká kritéria jsou vhodná ke klasifikaci hvězd horní části hlavní
... piece of information needed to identify larger celestial systems and structures, for instance determining the radial velocity or the rate of rotation. However, to gain this information, we need to classify the star most of the time, in order to determine what its spectra look like without the variou ...
... piece of information needed to identify larger celestial systems and structures, for instance determining the radial velocity or the rate of rotation. However, to gain this information, we need to classify the star most of the time, in order to determine what its spectra look like without the variou ...
Blue horizontal branch stars in the Sloan Digital Sky Survey:
... Photo version 5.4.25 (2003 June). The psf magnitudes are currently accurate to about 2% in g, r, and i and 3-5% in u and z for bright (< 20 mag) point sources. The SDSS is 50% complete for point sources to (u, g, r, i, z) = (22.5, 23.2, 22.6, 21.9, 20.8), and the full-width at half-maximum (FWHM) of ...
... Photo version 5.4.25 (2003 June). The psf magnitudes are currently accurate to about 2% in g, r, and i and 3-5% in u and z for bright (< 20 mag) point sources. The SDSS is 50% complete for point sources to (u, g, r, i, z) = (22.5, 23.2, 22.6, 21.9, 20.8), and the full-width at half-maximum (FWHM) of ...
An improved classification of B[e]-type stars
... spectrum and should not automatically be extended to other wavelength regions. For instance, the ISO − SW S spectrum of many luminous supergiants show the emission line of [Fe ii] at λ25.99 µm. If this were taken as an indication of the B[e] phenomenon, the class of stars that show the B[e] phenomen ...
... spectrum and should not automatically be extended to other wavelength regions. For instance, the ISO − SW S spectrum of many luminous supergiants show the emission line of [Fe ii] at λ25.99 µm. If this were taken as an indication of the B[e] phenomenon, the class of stars that show the B[e] phenomen ...
Probability of Solar Flares Turn Out to Form a Coronal Mass
... The existence of a clear correlation between the observed radio flux and solar activity was found since the first observations of solar radio emission in the late 1940‟s [1]. The study of solar flares and CMEs variations from the corona magnetic region is the most active manifestation of solar activ ...
... The existence of a clear correlation between the observed radio flux and solar activity was found since the first observations of solar radio emission in the late 1940‟s [1]. The study of solar flares and CMEs variations from the corona magnetic region is the most active manifestation of solar activ ...
Exploring Strange New Worlds: From Giant Planets to Super Earths
... Science fiction portrays our Milky Way Galaxy as filled with habitable planets populated by advanced civilizations engaged in interstellar trade and !conflict. !Back in our real universe, Earth-like planets and alien life have proved elusive. !Has science fiction led us astray? !NASA recently launch ...
... Science fiction portrays our Milky Way Galaxy as filled with habitable planets populated by advanced civilizations engaged in interstellar trade and !conflict. !Back in our real universe, Earth-like planets and alien life have proved elusive. !Has science fiction led us astray? !NASA recently launch ...
Observation of Neutrinos at Super-Kamiokande Observatory
... properties has been obtained over these last 20 years, but there are still things that are not understood. For example, which of neutrinos 1 and 3 in Figure 3 is heavier is not known. In addition, it is still not known whether neutrinos and antineutrinos oscillate in exactly the same way. Furthermor ...
... properties has been obtained over these last 20 years, but there are still things that are not understood. For example, which of neutrinos 1 and 3 in Figure 3 is heavier is not known. In addition, it is still not known whether neutrinos and antineutrinos oscillate in exactly the same way. Furthermor ...
discovery of four new massive and dense cold cores
... Surveys of molecular line emission in high-density tracers ( Plume et al. 1992, 1997; Juvela 1996) and of dust continuum emission ( Beuther et al. 2002; Mueller et al. 2002) made with single-dish telescopes have shown that massive stars form in regions of molecular gas with distinctive physical para ...
... Surveys of molecular line emission in high-density tracers ( Plume et al. 1992, 1997; Juvela 1996) and of dust continuum emission ( Beuther et al. 2002; Mueller et al. 2002) made with single-dish telescopes have shown that massive stars form in regions of molecular gas with distinctive physical para ...
400 YEARS OF STELLAR ROTATION - DFTE
... Earth, Jupiter had four satellites (Moons), Venus had phases like the Moon, Saturn had some sort of “ears” and finally sunspots and solar rotation (summer 1610 ?). The first results about the Moon, the multitude of stars in clouds and Jupiter satellites, were published in the space of a few months i ...
... Earth, Jupiter had four satellites (Moons), Venus had phases like the Moon, Saturn had some sort of “ears” and finally sunspots and solar rotation (summer 1610 ?). The first results about the Moon, the multitude of stars in clouds and Jupiter satellites, were published in the space of a few months i ...
Physical Properties of Wolf-Rayet Stars
... galaxies, they are the prime candidates for the immediate progenitors of long, soft gamma-ray bursts (GRBs, Woosley & Bloom 2006), and they provide a signature of high-mass star formation in galaxies (Schaerer & Vacca 1998). Spectroscopically, WR stars are spectacular in appearance, with strong, bro ...
... galaxies, they are the prime candidates for the immediate progenitors of long, soft gamma-ray bursts (GRBs, Woosley & Bloom 2006), and they provide a signature of high-mass star formation in galaxies (Schaerer & Vacca 1998). Spectroscopically, WR stars are spectacular in appearance, with strong, bro ...
LIGO and the MIT Kavli Institute no illustrations
... physics reach that during its first several hours of operation will exceed the integrated observations of the 1 year initial LIGO Science Run. These improvements will enable the next generation of interferometers to study sources not accessible to initial LIGO, and to extract detailed astrophysical ...
... physics reach that during its first several hours of operation will exceed the integrated observations of the 1 year initial LIGO Science Run. These improvements will enable the next generation of interferometers to study sources not accessible to initial LIGO, and to extract detailed astrophysical ...
- REAL-J
... 4623 C. WETTERER, S. MAJCEN, D. BURTZ: GSC 223:1761 { A New Delta Scuti Variable Star in Cancer : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : 1 { 3 4624 LEROY F. SNYDER: Period Change in UV Leonis : : : : : : : : : : : : : : : : : : : : : : : : 1 { 4 462 ...
... 4623 C. WETTERER, S. MAJCEN, D. BURTZ: GSC 223:1761 { A New Delta Scuti Variable Star in Cancer : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : 1 { 3 4624 LEROY F. SNYDER: Period Change in UV Leonis : : : : : : : : : : : : : : : : : : : : : : : : 1 { 4 462 ...
Present
... objects, so that the average starburst properties of the bulk of this class remain undetermined. We have been awarded 39h of MAMBO observations to observe an unbiased complete random sample, which has excellent X-ray and optical coverage, to determine the average value of S(1.2mm) and inferred quant ...
... objects, so that the average starburst properties of the bulk of this class remain undetermined. We have been awarded 39h of MAMBO observations to observe an unbiased complete random sample, which has excellent X-ray and optical coverage, to determine the average value of S(1.2mm) and inferred quant ...
Follow-up observations of extremely metal
... Context. The most metal-poor stars in the Milky Way witnessed the early phases of formation of the Galaxy, and have chemical ...
... Context. The most metal-poor stars in the Milky Way witnessed the early phases of formation of the Galaxy, and have chemical ...
Time evolution and rotation of starspots on CoRoT
... The location in time of a “bump” along the transit light curve provides unambiguous information on the longitude of the corresponding spot. When the spot latitude is fixed a priori, the radius and the intensity of the spot may show some degree of degeneracy, but in the case of a highly accurate ligh ...
... The location in time of a “bump” along the transit light curve provides unambiguous information on the longitude of the corresponding spot. When the spot latitude is fixed a priori, the radius and the intensity of the spot may show some degree of degeneracy, but in the case of a highly accurate ligh ...
Polaris B, an optical companion of Polaris (alpha UMi) system
... optical companions, Polaris C and D (13 and 12m , angular separations from Polaris A of 43 and 83 , respectively, are also potential members of the multiple system (Fernie, 1966), although recent observations refute that suggestion (Evans et al., 2007). It would therefore be interesting to establish ...
... optical companions, Polaris C and D (13 and 12m , angular separations from Polaris A of 43 and 83 , respectively, are also potential members of the multiple system (Fernie, 1966), although recent observations refute that suggestion (Evans et al., 2007). It would therefore be interesting to establish ...
Session 1: Stellar winds, diagnostics across the electromagnetic
... Detectable radio emission occurs during all phases of massive star evolution.I will concentrate on the thermal and non-thermal continuum emission from early-type stars. The thermal radio emission is due to free-free interactions in the ionized stellar wind material. Early ideas that this would lead ...
... Detectable radio emission occurs during all phases of massive star evolution.I will concentrate on the thermal and non-thermal continuum emission from early-type stars. The thermal radio emission is due to free-free interactions in the ionized stellar wind material. Early ideas that this would lead ...
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.