Quantum Optics and Photon Correlations in Astronomical
... comparable with extending the detectable frequencies in astronomy to infrared light and X-rays, or the development of photometers with microsecond resolution. We think that maybe astronomy has neglected g (2) for longer than was strictly necessary from a technological point of view. It is always eas ...
... comparable with extending the detectable frequencies in astronomy to infrared light and X-rays, or the development of photometers with microsecond resolution. We think that maybe astronomy has neglected g (2) for longer than was strictly necessary from a technological point of view. It is always eas ...
The dense gas mass fraction in the W51 cloud and its protoclusters
... for decades (Mangum & Wootten 1993). The centimeter lines, H2 CO 110 −111 (6.2 cm, 4.82966 GHz) and 211 −212 (2.1 cm, 14.48848 GHz), have a peculiar excitation process in which collisions overpopulate the lower of the two Kc rotational states, where Kc is the quantum number representing the angular ...
... for decades (Mangum & Wootten 1993). The centimeter lines, H2 CO 110 −111 (6.2 cm, 4.82966 GHz) and 211 −212 (2.1 cm, 14.48848 GHz), have a peculiar excitation process in which collisions overpopulate the lower of the two Kc rotational states, where Kc is the quantum number representing the angular ...
Detection and characterization of extrasolar planets: the
... transit around a bright star requires a telescope as small as 20-cm in diameter, and many transit surveys were initiated after this first success; 2) studies of a planetary system seen edge-on is much richer than for systems at any inclination, because the radius and the mass are directly measured. ...
... transit around a bright star requires a telescope as small as 20-cm in diameter, and many transit surveys were initiated after this first success; 2) studies of a planetary system seen edge-on is much richer than for systems at any inclination, because the radius and the mass are directly measured. ...
astronomy beat - Astronomical Society of the Pacific
... sometimes they put on a great show. But not Elenin. Right now that comet looks kind of wimpy. Some cometary visitors arriving from beyond the planetary region —like Hale-Bopp in 1997 — have really lit up the night sky where you can see them easily with the naked eye. But Elenin is trending toward t ...
... sometimes they put on a great show. But not Elenin. Right now that comet looks kind of wimpy. Some cometary visitors arriving from beyond the planetary region —like Hale-Bopp in 1997 — have really lit up the night sky where you can see them easily with the naked eye. But Elenin is trending toward t ...
Descending from on high: Lyman-series cascades and spin
... Rees 1990) that neutral hydrogen in the intergalactic medium (IGM) may be detectable in emission or absorption against the cosmic microwave background (CMB) at the wavelength of the redshifted 21-cm line, the spin-flip transition between the singlet and triplet hyperfine levels of the hydrogen groun ...
... Rees 1990) that neutral hydrogen in the intergalactic medium (IGM) may be detectable in emission or absorption against the cosmic microwave background (CMB) at the wavelength of the redshifted 21-cm line, the spin-flip transition between the singlet and triplet hyperfine levels of the hydrogen groun ...
orion® starseekers - NexStar Resource Site
... length (i.e., the smaller the number), the higher the magnification. Generally, you will use low-to-moderate power when viewing. For more information on how to determine power, see the section on “Calculating Magnification.” Barrel diameter is the diameter of the barrel that slides into the star dia ...
... length (i.e., the smaller the number), the higher the magnification. Generally, you will use low-to-moderate power when viewing. For more information on how to determine power, see the section on “Calculating Magnification.” Barrel diameter is the diameter of the barrel that slides into the star dia ...
Dependences of the group velocity for
... Many interests have been focused on manipulating the group velocity of light pulses [1–4]. Its main goals include the understanding of physical laws for light pulse propagation as well as many promising applications such as controllable optical delay lines, all-optical memories, and data resynchroni ...
... Many interests have been focused on manipulating the group velocity of light pulses [1–4]. Its main goals include the understanding of physical laws for light pulse propagation as well as many promising applications such as controllable optical delay lines, all-optical memories, and data resynchroni ...
LEP 2.6.07 Helium Neon Laser
... The four sub-states of the 2s group are all populated in a similar way. Visible (VIS) optical transitions and laser processes take place between the 3s2 R 2pi and infrared (IR) transitions between the 2si R 2pi energy levels. The following table shows the most important laser transitions. The Einste ...
... The four sub-states of the 2s group are all populated in a similar way. Visible (VIS) optical transitions and laser processes take place between the 3s2 R 2pi and infrared (IR) transitions between the 2si R 2pi energy levels. The following table shows the most important laser transitions. The Einste ...
Life and Death of Stars
... "Seeing into the Heart of Mira A and its Partner" by ESO/S. Ramstedt (Uppsala University, Sweden) & W. Vlemmings (Chalmers University of Technology, Sweden) http://www.eso.org/public/images/potw1447a/. Licensed under CC BY 4.0 via Wikimedia Commons http://commons.wikimedia.org/wiki/File:Seeing_into_ ...
... "Seeing into the Heart of Mira A and its Partner" by ESO/S. Ramstedt (Uppsala University, Sweden) & W. Vlemmings (Chalmers University of Technology, Sweden) http://www.eso.org/public/images/potw1447a/. Licensed under CC BY 4.0 via Wikimedia Commons http://commons.wikimedia.org/wiki/File:Seeing_into_ ...
Two New Triple Star Systems with Detectable Inner Orbital Motions
... to 1994. These cover an arc of about 60 degrees and show a well-defined orbital arc. After 1994, the inner system unfortunately could not be resolved. But this suborbital motion is detectable in the residuals of the outer system STF162 AB (Figure 2), so we determined a provisional period of the inte ...
... to 1994. These cover an arc of about 60 degrees and show a well-defined orbital arc. After 1994, the inner system unfortunately could not be resolved. But this suborbital motion is detectable in the residuals of the outer system STF162 AB (Figure 2), so we determined a provisional period of the inte ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... (1986), and we orient the reader to these papers for these objects. The present review will focus on the low-mass part of the MF in various regions of the Galaxy and its extension into the substellar regime. Low-mass stars (hereafter stars with mass m ! 1 M,) have effective temperatures Tef f " 6000 ...
... (1986), and we orient the reader to these papers for these objects. The present review will focus on the low-mass part of the MF in various regions of the Galaxy and its extension into the substellar regime. Low-mass stars (hereafter stars with mass m ! 1 M,) have effective temperatures Tef f " 6000 ...
Lecture0006c - Purdue University Cytometry Laboratories
... DCXR -- dichroic long pass, extended reflection DCXRU -- dichroic longpass, extended reflection including the UV PC -- polychroic beamsplitter. This is a beamsplitter that reflects and transmits more than two bands of light. GG -- Green Glass. Longpass absorption glass from Schott Glassworks with cu ...
... DCXR -- dichroic long pass, extended reflection DCXRU -- dichroic longpass, extended reflection including the UV PC -- polychroic beamsplitter. This is a beamsplitter that reflects and transmits more than two bands of light. GG -- Green Glass. Longpass absorption glass from Schott Glassworks with cu ...
A Collimated Jet and an Infalling-Rotating Disk in G192.16−3.84
... explosion may have occurred when these stellar objects were located in the common point with strong dynamical interactions (Bally, Zinnecker 2005). However, the stellar volume density requested for this scenario (> 107 pc−3 ) should predict a high frequency of such a runaway collapse and explosion e ...
... explosion may have occurred when these stellar objects were located in the common point with strong dynamical interactions (Bally, Zinnecker 2005). However, the stellar volume density requested for this scenario (> 107 pc−3 ) should predict a high frequency of such a runaway collapse and explosion e ...
“XRbinary”: A Program to Calculate the Orbital Light Curves of X
... stars, and P is the orbital period. Star 1, the “primary star,” is surrounded by an accretion disk. Star 2 is called the “secondary star.” Because the program is optimized for calculating the light curves of X-ray binary stars, it has several distinctive features: • The secondary star is assumed to ...
... stars, and P is the orbital period. Star 1, the “primary star,” is surrounded by an accretion disk. Star 2 is called the “secondary star.” Because the program is optimized for calculating the light curves of X-ray binary stars, it has several distinctive features: • The secondary star is assumed to ...
Astronomy
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
The evolution of massive stars and their spectra
... observables of massive stars can be strongly influenced by a radiatively driven stellar wind that is characteristic of these stars. The effects of mass loss on the observables depend on the initial mass and metallicity, since they are in general more noticeable in MS stars with large initial masses, ...
... observables of massive stars can be strongly influenced by a radiatively driven stellar wind that is characteristic of these stars. The effects of mass loss on the observables depend on the initial mass and metallicity, since they are in general more noticeable in MS stars with large initial masses, ...
Radio properties of a complete sample of nearby groups of galaxies
... low-frequency GMRT radio images of the nearby (<80 Mpc) central brightest group ellipticals from the high richness CLoGS sub-sample are presented for the first time at 235 and 610 MHz. Using the sensitivity to older electron populations at 235 MHz and the resolution of 610 MHz as a key to identify p ...
... low-frequency GMRT radio images of the nearby (<80 Mpc) central brightest group ellipticals from the high richness CLoGS sub-sample are presented for the first time at 235 and 610 MHz. Using the sensitivity to older electron populations at 235 MHz and the resolution of 610 MHz as a key to identify p ...
CENTRAL TEXAS COLLEGE
... distinguish among conductors, semiconductors and insulators define ion and give several ways of producing ionization explain why grounding the metal shell of an electrical appliance makes its use safer define superconductivity and discuss its potential importance describe electric current and potent ...
... distinguish among conductors, semiconductors and insulators define ion and give several ways of producing ionization explain why grounding the metal shell of an electrical appliance makes its use safer define superconductivity and discuss its potential importance describe electric current and potent ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.