Terahertz Electromagnetic Waves Properties and
... Terahertz waves are quickly gaining attention and research funding. These waves are in the 100 GHz to 10 THz frequency range, this range is also know as the “terahertz gap,” as demonstrated in figure 1. This gap exists because until recently effective methods of generating controlled THz waves, and ...
... Terahertz waves are quickly gaining attention and research funding. These waves are in the 100 GHz to 10 THz frequency range, this range is also know as the “terahertz gap,” as demonstrated in figure 1. This gap exists because until recently effective methods of generating controlled THz waves, and ...
PDF Book "PHYSICS I: Oscillations and Waves"
... The book “Oscillations and waves” is an account of one semester course, PHYSICS-I, given by the authors for the last three years at IIT, Kharagpur. The book is targeted at the first year undergraduate science and engineering students. Starting with oscillations in general, the book moves to interfer ...
... The book “Oscillations and waves” is an account of one semester course, PHYSICS-I, given by the authors for the last three years at IIT, Kharagpur. The book is targeted at the first year undergraduate science and engineering students. Starting with oscillations in general, the book moves to interfer ...
Measuring the orbital periods of low mass X-ray binaries in the X
... curve. However, the X-ray data can be recorded as an event list that provides the event arrival times for the detected X-ray photons. The Z-test (Buccheri et al. 1983) and H-test (de Jager et al. 1989) directly operate on the event arrival time without binning and a unique result can be obtained. In ...
... curve. However, the X-ray data can be recorded as an event list that provides the event arrival times for the detected X-ray photons. The Z-test (Buccheri et al. 1983) and H-test (de Jager et al. 1989) directly operate on the event arrival time without binning and a unique result can be obtained. In ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... metal itself were “light sources,” with an intensity proportional to the amount of uranium present; the chemical combination had no effect. Two years later, Pierre and Marie Curie coined the term “radioactive” for those elements that emitted such “Becquerel rays.” A year later, Ernest Rutherford dem ...
... metal itself were “light sources,” with an intensity proportional to the amount of uranium present; the chemical combination had no effect. Two years later, Pierre and Marie Curie coined the term “radioactive” for those elements that emitted such “Becquerel rays.” A year later, Ernest Rutherford dem ...
Observation of Neutrinos at Super-Kamiokande Observatory
... creating electrons, muons, and other charged particles. Measuring the Cherenkov light produced by particles created by such reactions enables information on the original neutrino such as flavor, energy, and interacted position to be reconstructed. Despite the scale of this detector, it can observe o ...
... creating electrons, muons, and other charged particles. Measuring the Cherenkov light produced by particles created by such reactions enables information on the original neutrino such as flavor, energy, and interacted position to be reconstructed. Despite the scale of this detector, it can observe o ...
Cyclotron waves in a non-neutral plasma column
... diagnose the charge to mass ratio and/or the relative concentration of plasma species1 (via the technique of “ioncyclotron mass spectrometry”). While most of these devices work in the low-density regime where plasma effects are small, cyclotron frequency shifts universally arise from electric fields ...
... diagnose the charge to mass ratio and/or the relative concentration of plasma species1 (via the technique of “ioncyclotron mass spectrometry”). While most of these devices work in the low-density regime where plasma effects are small, cyclotron frequency shifts universally arise from electric fields ...
Discovery of a bright quasar without a massive
... As a complementary approach, avoiding uncertainties related to the black hole mass estimates, we compare directly our upper limits to the magnitudes measured for typical quasar host galaxies. We use the HST sample of 17 quasar host galaxies from Floyd et al.8. After conversion of their values to our ...
... As a complementary approach, avoiding uncertainties related to the black hole mass estimates, we compare directly our upper limits to the magnitudes measured for typical quasar host galaxies. We use the HST sample of 17 quasar host galaxies from Floyd et al.8. After conversion of their values to our ...
Cycle No.33 - NCRA-TIFR
... Committee (GTAC), which will make recommendations for allocation of observing time for each proposal. 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 ...
... Committee (GTAC), which will make recommendations for allocation of observing time for each proposal. 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 ...
The Milky Way-Pulsars and Isolated Neutron Stars
... on old V-2 (captured in Germany after the World War II) and Aerobee rockets, they were the first who detected X-rays from the very hot gas in the solar corona. However, the intensity of this radiation was found to be a factor 106 lower than that measured at optical wavelengths. In the late 1 X-rays ...
... on old V-2 (captured in Germany after the World War II) and Aerobee rockets, they were the first who detected X-rays from the very hot gas in the solar corona. However, the intensity of this radiation was found to be a factor 106 lower than that measured at optical wavelengths. In the late 1 X-rays ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
Super and massive AGB stars-IV. Final fates
... upon the choice of mass-loss rate. In general, defining the lowest mass for gravitational collapse supernovae is of considerable interest (e.g. Heger et al. 2003; Eldridge & Tout 2004; Ibeling & Heger 2013) and the numerous problems which hamper the accurate determination of this boundary, both theo ...
... upon the choice of mass-loss rate. In general, defining the lowest mass for gravitational collapse supernovae is of considerable interest (e.g. Heger et al. 2003; Eldridge & Tout 2004; Ibeling & Heger 2013) and the numerous problems which hamper the accurate determination of this boundary, both theo ...
Chapter 17
... waves were emanating from the jet and the main body of the object. 2. The spectra of 3C 273 and 3C 48 (the second unusual object discovered in 1960) showed emission lines, which could not be identified. Because of their star-like appearance and strong radio emission, the objects were named quasars. ...
... waves were emanating from the jet and the main body of the object. 2. The spectra of 3C 273 and 3C 48 (the second unusual object discovered in 1960) showed emission lines, which could not be identified. Because of their star-like appearance and strong radio emission, the objects were named quasars. ...
Multiple origins of asteroid pairs
... systems stray from the predicted relation, and Pravec et al. (2010) explored how changes in the spherical approximation may account for these discrepancies. In particular, asserting that the components have different shapes changes the initial free energy system since the critical spin rate for rota ...
... systems stray from the predicted relation, and Pravec et al. (2010) explored how changes in the spherical approximation may account for these discrepancies. In particular, asserting that the components have different shapes changes the initial free energy system since the critical spin rate for rota ...
Binary evolution using the theory of osculating orbits
... STAREVOL. Details on the stellar input physics can be found in Siess (2010), and references therein, while the binary input physics is described in Siess et al. (2013) and Deschamps et al. (2013). In this section we present our new implementation of the osculating scheme. 2.1. Variation of the orbit ...
... STAREVOL. Details on the stellar input physics can be found in Siess (2010), and references therein, while the binary input physics is described in Siess et al. (2013) and Deschamps et al. (2013). In this section we present our new implementation of the osculating scheme. 2.1. Variation of the orbit ...
16 Neutrino Oscillations
... that neutrinos were, in fact, massless. We now know they have a very small mass, the current limits are mν < 2 eV however values for the absolute masses are unknown. The mass eigenstates of the neutrinos are not identical to the flavour eigenstates. The flavour eigenstates are νe , νµ , ντ ; these a ...
... that neutrinos were, in fact, massless. We now know they have a very small mass, the current limits are mν < 2 eV however values for the absolute masses are unknown. The mass eigenstates of the neutrinos are not identical to the flavour eigenstates. The flavour eigenstates are νe , νµ , ντ ; these a ...
Slide 1
... The Life of a Heavy Star • For heavy stars the first part of their life is the same as for lighter stars: after the hydrogen runs out, gravity crushes the core • What is different is that for heavy stars there is so much mass that gravity can continue to crush the core, and the temperature can rise ...
... The Life of a Heavy Star • For heavy stars the first part of their life is the same as for lighter stars: after the hydrogen runs out, gravity crushes the core • What is different is that for heavy stars there is so much mass that gravity can continue to crush the core, and the temperature can rise ...
UNIVERSITY OF PADUA Master degree in
... Direct detection of H2 can be observed through ultraviolet absorption, but due to the opaqueness in the ultraviolet band of the Earth’s atmosphere these observations must be done from space [36]. A more common indirect observation of H2 is through radio and sub millimeter emission from dust grains o ...
... Direct detection of H2 can be observed through ultraviolet absorption, but due to the opaqueness in the ultraviolet band of the Earth’s atmosphere these observations must be done from space [36]. A more common indirect observation of H2 is through radio and sub millimeter emission from dust grains o ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... The first quasars were discovered with radio telescopes in the late 1950s, recorded as radio sources with no corresponding visible object. Further investigation found that many had unusually small angular sizes, which on a photographic plate would appear as the image of a star. When the spectra of t ...
... The first quasars were discovered with radio telescopes in the late 1950s, recorded as radio sources with no corresponding visible object. Further investigation found that many had unusually small angular sizes, which on a photographic plate would appear as the image of a star. When the spectra of t ...