L53 He I 1.083 mm EMISSION AND ABSORPTION IN DG TAURI
... coincide with a high-velocity component of the [Fe ii] 1.257 mm emission, which arises from a jet within an arcsecond of the star. The presence of such a high-excitation line (with an excitation energy of ∼20 eV) within the jet supports the scenario of shock heating. The bright He i component does n ...
... coincide with a high-velocity component of the [Fe ii] 1.257 mm emission, which arises from a jet within an arcsecond of the star. The presence of such a high-excitation line (with an excitation energy of ∼20 eV) within the jet supports the scenario of shock heating. The bright He i component does n ...
The Spectra of Stars
... Hot, dense lower photosphere of a star is dense lower photosphere of a star is surrounded by thinner (but still fairly hot) atmosphere. atmosphere – Produces an Absorption Line spectrum. – Lines come from the elements in the stellar Lines come from the elements in the stellar atmosphere. ...
... Hot, dense lower photosphere of a star is dense lower photosphere of a star is surrounded by thinner (but still fairly hot) atmosphere. atmosphere – Produces an Absorption Line spectrum. – Lines come from the elements in the stellar Lines come from the elements in the stellar atmosphere. ...
Data-mining in astrophysics. A search for new variable stars in
... (Conference talk) Abstract. A review of already known algorithms for search of variable objects in large databases is presented and a new multi parametric data-mining method is proposed. This method was tested on NSVS database using "relative" amplitude of light curve and maximum intensity of power ...
... (Conference talk) Abstract. A review of already known algorithms for search of variable objects in large databases is presented and a new multi parametric data-mining method is proposed. This method was tested on NSVS database using "relative" amplitude of light curve and maximum intensity of power ...
The Present Status of Chinese Study of Solar Eclipses
... Mr. Zhu Wenxin is the first scholar who studied all the solar-eclipse records in Chinese history with modern astronomical computational method, and he published the book, An Examination on History Records of Solar Eclipse (Zhu Wenxin, 1934). A total of 921 records are sorted out in this book. Zhu in ...
... Mr. Zhu Wenxin is the first scholar who studied all the solar-eclipse records in Chinese history with modern astronomical computational method, and he published the book, An Examination on History Records of Solar Eclipse (Zhu Wenxin, 1934). A total of 921 records are sorted out in this book. Zhu in ...
A Search For The Transit Of HD 168443b: Improved Orbital
... The number of known exoplanets has grown rapidly in the last decade, with over 600 confirmed exoplanets known to date.13 While most of these planets have been discovered using radial velocity (RV) techniques, the number of known transiting planets has increased significantly due to dedicated transit ...
... The number of known exoplanets has grown rapidly in the last decade, with over 600 confirmed exoplanets known to date.13 While most of these planets have been discovered using radial velocity (RV) techniques, the number of known transiting planets has increased significantly due to dedicated transit ...
Cycle No.33 - NCRA-TIFR
... Current technical details about the GMRT, such as modes of operation, available frequency bands and usable bandwidths, system parameters and expected performance, as well as facilities for absentee observing for users, can be found in the GMRT Specifications and Status document at http://www.ncra.ti ...
... Current technical details about the GMRT, such as modes of operation, available frequency bands and usable bandwidths, system parameters and expected performance, as well as facilities for absentee observing for users, can be found in the GMRT Specifications and Status document at http://www.ncra.ti ...
“End-of-the-Line” W UMa Eclipsing Binary V523
... the W Ursae Majoris (W UMa) class where the dominant energy transport mechanism within the common envelope is convection—similar to the situation in the outer layers of the Sun. In these binaries, significant energy is transferred from the higher mass star to the lower mass star, resulting in a near ...
... the W Ursae Majoris (W UMa) class where the dominant energy transport mechanism within the common envelope is convection—similar to the situation in the outer layers of the Sun. In these binaries, significant energy is transferred from the higher mass star to the lower mass star, resulting in a near ...
Observations and analysis of phase scintillation of spacecraft signal
... takes the electron density in fast and slow wind into account. The calculated TEC values for the Mars and Venus orbits are shown with respect to solar elongation angle in Fig. 1. Although this work focusses on VEX, we included data for Mars since MEX can also be used for interplanetary plasma studie ...
... takes the electron density in fast and slow wind into account. The calculated TEC values for the Mars and Venus orbits are shown with respect to solar elongation angle in Fig. 1. Although this work focusses on VEX, we included data for Mars since MEX can also be used for interplanetary plasma studie ...
Astrophysics
... emission from extremely energetic electrons, giving information on the shock acceleration process which is probably responsible for producing galactic cosmic rays. Prof. Ellison studies the acceleration of these particles via the Diffusive Shock Acceleration mechanism including nonlinear effects of ...
... emission from extremely energetic electrons, giving information on the shock acceleration process which is probably responsible for producing galactic cosmic rays. Prof. Ellison studies the acceleration of these particles via the Diffusive Shock Acceleration mechanism including nonlinear effects of ...
A Solar Polar Imager Concept - The National Academies of
... potential SPI, complemented by near-Earth magnetograph observations, would enable us to follow the evolution of active regions for much longer than the half-solar rotation now possible. Figure 4 Closed circulation lines: Possible streamWith only observations from Earth, each lines of meridional flow ...
... potential SPI, complemented by near-Earth magnetograph observations, would enable us to follow the evolution of active regions for much longer than the half-solar rotation now possible. Figure 4 Closed circulation lines: Possible streamWith only observations from Earth, each lines of meridional flow ...
Stellar Spectra Classification
... Stellar Spectra Classification Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can be affected by its distance from the observer, its size, or by the presence of interstellar dust. Instead, astronomers classify stars based on the major compon ...
... Stellar Spectra Classification Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can be affected by its distance from the observer, its size, or by the presence of interstellar dust. Instead, astronomers classify stars based on the major compon ...
PDF - Isaac Scientific Publishing
... 1986. However, at that time the finding place in Iraq of the cylinder seal was not known to me because I had only seen it in a popular science book without references, and it was not obvious at that time that my new computer program for calculation of ancient solar eclipses was good enough. Therefor ...
... 1986. However, at that time the finding place in Iraq of the cylinder seal was not known to me because I had only seen it in a popular science book without references, and it was not obvious at that time that my new computer program for calculation of ancient solar eclipses was good enough. Therefor ...
Five New Giant Exoplanets from the California
... Among the 1800 FGKM stars we monitor at the Keck telescope for giant planets, 1330 of them have been monitored from 1997 to the present with a precision of 1– 3 m s−1 . The sample contains a nearly volume-limited sample of stars within five bins of B − V color, between 0.60 and 1.5. It is nearly dev ...
... Among the 1800 FGKM stars we monitor at the Keck telescope for giant planets, 1330 of them have been monitored from 1997 to the present with a precision of 1– 3 m s−1 . The sample contains a nearly volume-limited sample of stars within five bins of B − V color, between 0.60 and 1.5. It is nearly dev ...
Astronomy Astrophysics - Centro de Astrofísica da Universidade do
... The observations with the 1.0 m JKT (La Palma, Canary Islands, Spain) were carried out during NovemberDecember 2001 using the JAG CCD camera equipped with the 2048 × 2048 pix2 SITe2 detector, providing a 11 × 11 arcmin2 field of view and a pixel scale of 0.33 arcsec/pixel. A Johnson V-band filter wa ...
... The observations with the 1.0 m JKT (La Palma, Canary Islands, Spain) were carried out during NovemberDecember 2001 using the JAG CCD camera equipped with the 2048 × 2048 pix2 SITe2 detector, providing a 11 × 11 arcmin2 field of view and a pixel scale of 0.33 arcsec/pixel. A Johnson V-band filter wa ...
San Diego Astronomy Association CONTENTS
... evolved binary stars, a red dwarf (RD) and a white dwarf (WD) in very close orbits with orbital times of 1-10 hours. I have measured the light from eclipses of CV's. Some images and materials are not able to be included in the Newsletter, but can be found on the SDAA web site at: http://sdaa.org/SDA ...
... evolved binary stars, a red dwarf (RD) and a white dwarf (WD) in very close orbits with orbital times of 1-10 hours. I have measured the light from eclipses of CV's. Some images and materials are not able to be included in the Newsletter, but can be found on the SDAA web site at: http://sdaa.org/SDA ...
Neutron Density and Neutron Source Determination in Barium
... parameters, a poor determination of the C 2 strength, or the presence of unknown blends. The latter source of error is the most likely in view of the cool nature of the star under study. In light of these uncertainties it is important to check these results using another portion of the stellar spect ...
... parameters, a poor determination of the C 2 strength, or the presence of unknown blends. The latter source of error is the most likely in view of the cool nature of the star under study. In light of these uncertainties it is important to check these results using another portion of the stellar spect ...
L103 A NEW MILKY WAY DWARF SATELLITE IN CANES
... Fig. 7 of McConnachie & Irwin 2006), suggesting that this correlation may be at least partially due to observational biases (e.g., Willman et al. 2004). A search of the SDSS DR5 spectroscopic database revealed the spectrum of a CH carbon star, SDSS J132755.56⫹333521.7, in close proximity to the cent ...
... Fig. 7 of McConnachie & Irwin 2006), suggesting that this correlation may be at least partially due to observational biases (e.g., Willman et al. 2004). A search of the SDSS DR5 spectroscopic database revealed the spectrum of a CH carbon star, SDSS J132755.56⫹333521.7, in close proximity to the cent ...
TWO NEW VARIABLE STARS OBSERVED IN THE FIELD OF THE
... two normal stars, one that is cooler and brighter in red/near-infrared bands -then determining the observed high value for the V-K index- while the hotter companion is brigther at shorter wavelenghts, producing a V-R index shifted towards an upper spectral class. As a further check to support our in ...
... two normal stars, one that is cooler and brighter in red/near-infrared bands -then determining the observed high value for the V-K index- while the hotter companion is brigther at shorter wavelenghts, producing a V-R index shifted towards an upper spectral class. As a further check to support our in ...
Morphological characteristics of OB spectra and environments
... λλ4647–4650–4652 emission lines comparable to N III λλ4634–4640–4642, they showed evidence of circumstellar activity in terms of sharp absorption features and P Cygni profiles at H and He I lines. During the past decade, all three have been shown to be extreme, periodic spectrum variables, and soon ...
... λλ4647–4650–4652 emission lines comparable to N III λλ4634–4640–4642, they showed evidence of circumstellar activity in terms of sharp absorption features and P Cygni profiles at H and He I lines. During the past decade, all three have been shown to be extreme, periodic spectrum variables, and soon ...
AN INTERSTELLAR CLOUD WITH A HIGH CON
... CN line, R(O) of the (0, 0) band in the B 2 ~+---? X 2 ~+ systellJ, at "A 3874.61 A, as measured by Dunham (194J) in seven stars, does not exceed 7 mA in strength, while the R(l) line at "A 3874.00 A is between two and three times weaker and the P(l) line is only marginally detected. The absorption ...
... CN line, R(O) of the (0, 0) band in the B 2 ~+---? X 2 ~+ systellJ, at "A 3874.61 A, as measured by Dunham (194J) in seven stars, does not exceed 7 mA in strength, while the R(l) line at "A 3874.00 A is between two and three times weaker and the P(l) line is only marginally detected. The absorption ...
Beatrice Muriel Hill Tinsley
... but somehow they were not very interested, and colleagues began to suspect that Beatrice might be movable. She received offers from the University of Chicago and elsewhere, and in 1975 accepted an associated professorship at Yale, where Richard Larson, with whom she had already carried out several p ...
... but somehow they were not very interested, and colleagues began to suspect that Beatrice might be movable. She received offers from the University of Chicago and elsewhere, and in 1975 accepted an associated professorship at Yale, where Richard Larson, with whom she had already carried out several p ...
Fulltext PDF
... that the pearly white corona was strongly polarized. This observation indicated the presence of material particles in the corona (to scatter the photospheric light). Today we know that scattering by the electrons in the corona is the reason for this polarization, but in 1868 electron was not yet dis ...
... that the pearly white corona was strongly polarized. This observation indicated the presence of material particles in the corona (to scatter the photospheric light). Today we know that scattering by the electrons in the corona is the reason for this polarization, but in 1868 electron was not yet dis ...
PPT
... Infrared integral field spectroscopic observations of globules (cometary knots) in the Helix Nebula (NGC 7293) ...
... Infrared integral field spectroscopic observations of globules (cometary knots) in the Helix Nebula (NGC 7293) ...
Fe I/Fe II ionization equilibrium in cool stars: NLTE versus LTE
... In all previous NLTE calculations, the model atom of Fe I was build using measured energy levels. The experimental analysis of Nave et al. (1994) with later updates provided 965 energy levels for Fe I. A comparison with the calculated Fe I atomic structure (Kurucz (2007)) reveals that the system of ...
... In all previous NLTE calculations, the model atom of Fe I was build using measured energy levels. The experimental analysis of Nave et al. (1994) with later updates provided 965 energy levels for Fe I. A comparison with the calculated Fe I atomic structure (Kurucz (2007)) reveals that the system of ...
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.