The fate of black hole singularities and the parameters of the
... beginning with an initial value p∗ and letting the system evolve through N generations. Let us define a function B(p) on P that is the expected number of future singularities generated during a lifetime of a universe with parameters5 p. We may observe that, for most p, B(p) is one, but there are sma ...
... beginning with an initial value p∗ and letting the system evolve through N generations. Let us define a function B(p) on P that is the expected number of future singularities generated during a lifetime of a universe with parameters5 p. We may observe that, for most p, B(p) is one, but there are sma ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... interstellar medium, AGB stars are key players in the life cycle of dust and gas in the universe. However, a quantitative understanding of the mass-loss process is still largely lacking, particularly its dependence on metallicity. Aims. To investigate the relation between mass loss, luminosity and p ...
... interstellar medium, AGB stars are key players in the life cycle of dust and gas in the universe. However, a quantitative understanding of the mass-loss process is still largely lacking, particularly its dependence on metallicity. Aims. To investigate the relation between mass loss, luminosity and p ...
Search for an exosphere around 51 Pegasi B with ISO
... the atmosphere/exosphere of a large gas giant around 51 Peg. To detect signatures of an exosphere, we observed 51 Peg during transit phases of its planet. The same observations were then repeated at times when the planet was not in the line-ofsight. Table 1 provides the dates and times of our measur ...
... the atmosphere/exosphere of a large gas giant around 51 Peg. To detect signatures of an exosphere, we observed 51 Peg during transit phases of its planet. The same observations were then repeated at times when the planet was not in the line-ofsight. Table 1 provides the dates and times of our measur ...
On the elemental abundance and isotopic mixture of mercury in
... become selectively excited based on their velocities. For example, if the light flux is higher on the blue side of the line profile, then the particles moving in the direction of light propagation are excited more efficiently. The light flux can thus induce a flow of excited particles in one direction ...
... become selectively excited based on their velocities. For example, if the light flux is higher on the blue side of the line profile, then the particles moving in the direction of light propagation are excited more efficiently. The light flux can thus induce a flow of excited particles in one direction ...
Astronomical Geography: An Examination of the Early American
... In the 1814 edition of Modern Geography, Morse's section on " fixed stars" proposed larger numbers of stars than earlier geog raphies : " The fixed stars . .. are found to be collected in clusters. When a small magnifying power is used, these clusters appear like small light clouds, and hence have b ...
... In the 1814 edition of Modern Geography, Morse's section on " fixed stars" proposed larger numbers of stars than earlier geog raphies : " The fixed stars . .. are found to be collected in clusters. When a small magnifying power is used, these clusters appear like small light clouds, and hence have b ...
Binary Star Formation Part 2
... It appears that interactions in a cluster-forming environment may be the key to their formation Even though the transition in observable properties between close binaries and wide binaries is smooth, there are likely to be a number of different physical processes that produce close binaries ...
... It appears that interactions in a cluster-forming environment may be the key to their formation Even though the transition in observable properties between close binaries and wide binaries is smooth, there are likely to be a number of different physical processes that produce close binaries ...
Direct Imaging of Exoplanets - American Museum of Natural History
... Currently, the techniques of radial velocity (RV), transits, and gravitational lensing are more productive than direct imaging. Remarkably, these techniques, including astrometry and direct imaging, perform nearly independent roles for exoplanet science, so each of them is valuable. Radial velocity ...
... Currently, the techniques of radial velocity (RV), transits, and gravitational lensing are more productive than direct imaging. Remarkably, these techniques, including astrometry and direct imaging, perform nearly independent roles for exoplanet science, so each of them is valuable. Radial velocity ...
What To See Telescope(Jul-Sept) v1 - One
... locate specific major constellations. To help you get oriented, the last appendix includes three whole-sky maps that show the constellations as seen from mid-northern latitudes in July, August, and September. Your telescope may have come with at least two eyepieces, and you may have acquired one or ...
... locate specific major constellations. To help you get oriented, the last appendix includes three whole-sky maps that show the constellations as seen from mid-northern latitudes in July, August, and September. Your telescope may have come with at least two eyepieces, and you may have acquired one or ...
- Interactive Media Systems, TU Vienna
... The VCR is a multi-user learning environment exploiting principles of edutainment learning through entertaining. Knowledge about space is mediated by working together as a team to accomplish a space mission. A ...
... The VCR is a multi-user learning environment exploiting principles of edutainment learning through entertaining. Knowledge about space is mediated by working together as a team to accomplish a space mission. A ...
Telescopes in History
... of this was the construction of the largest refracting telescopes ever built. The 36 in (0.9 m) instrument was installed at LICK OBSERVATORY in 1888, and was followed by the 40 in (1 m) telescope at YERKES OBSERVATORY in 1897. The driving force behind the Yerkes project, George Ellery HALE (1868–193 ...
... of this was the construction of the largest refracting telescopes ever built. The 36 in (0.9 m) instrument was installed at LICK OBSERVATORY in 1888, and was followed by the 40 in (1 m) telescope at YERKES OBSERVATORY in 1897. The driving force behind the Yerkes project, George Ellery HALE (1868–193 ...
Full Program with Abstracts - CIERA
... function of size, orbital period, and host star properties. We've learned that every late-type star has at least one planet on average, that terrestrial-sized planets are more common than larger planets within 1 AU, and that the nearest, potentially habitable earth-sized planet is likely within 5pc. ...
... function of size, orbital period, and host star properties. We've learned that every late-type star has at least one planet on average, that terrestrial-sized planets are more common than larger planets within 1 AU, and that the nearest, potentially habitable earth-sized planet is likely within 5pc. ...
Astronomy Astrophysics - Niels Bohr Institutet
... attention has been given to a realistic treatment of statistical biases and error estimates, as standard techniques tend to underestimate these effects and introduce spurious features in the age distributions. Our ages agree well with those by Edvardsson et al. (1993), despite several astrophysical a ...
... attention has been given to a realistic treatment of statistical biases and error estimates, as standard techniques tend to underestimate these effects and introduce spurious features in the age distributions. Our ages agree well with those by Edvardsson et al. (1993), despite several astrophysical a ...
Homework #3, AST 1002
... (a) Their absolute magnitude depends on their period. (b) They are found in the galactic plane. (c) They pulse with periods of about one day or less. The correct answer(s) is(are) ____________. 16. Which of the following is (are) correct? (a) White dwarfs contain a super conducting material. (b) Ura ...
... (a) Their absolute magnitude depends on their period. (b) They are found in the galactic plane. (c) They pulse with periods of about one day or less. The correct answer(s) is(are) ____________. 16. Which of the following is (are) correct? (a) White dwarfs contain a super conducting material. (b) Ura ...
Signatures of Planets in Protoplanetary and Debris
... of circumstellar disks, has been developed already, the planet formation process is in major parts still under discussion. In particular, adequate constraints from observations are required in order to either verify or rule out currently discussed planet formation scenarios (e.g., Pollack et al. 199 ...
... of circumstellar disks, has been developed already, the planet formation process is in major parts still under discussion. In particular, adequate constraints from observations are required in order to either verify or rule out currently discussed planet formation scenarios (e.g., Pollack et al. 199 ...
The absence of CO from the dust peak around ϵ Eri
... the same orbital distance as the ring. A second, more massive (∼1 M J ) planet may also be orbiting the star at ∼3 au (Hatzes et al. 2000). The established core accretion theory of planet formation (e.g. Boss 2000) generally allows ∼108 yr for the formation of terrestrial planets, but requires gas g ...
... the same orbital distance as the ring. A second, more massive (∼1 M J ) planet may also be orbiting the star at ∼3 au (Hatzes et al. 2000). The established core accretion theory of planet formation (e.g. Boss 2000) generally allows ∼108 yr for the formation of terrestrial planets, but requires gas g ...
Test Ch. 27 Multiple Choice Identify the choice that best completes
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
X-ray activity cycle on the active ultra
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
3. Wavefront sensors - Caltech Optical Observatories
... with respect to the telescope primary by an amount depending on the field angle—this is similar to anisoplanatism caused by atmospheric aberrations at an altitude not conjugate to the DM. Finally, a third effect is DM-to-lenslet misregistration and scale errors. In the analysis, the telescope primar ...
... with respect to the telescope primary by an amount depending on the field angle—this is similar to anisoplanatism caused by atmospheric aberrations at an altitude not conjugate to the DM. Finally, a third effect is DM-to-lenslet misregistration and scale errors. In the analysis, the telescope primar ...
SPACETIME SINGULARITIES: The STORY of BLACK HOLES
... with the mass of the earth would have Rs ∼ 9mm! What this means is that we would have to cram the entire mass of the earth into a region of diameter less than 18mm (just over the size of a dime) before the gravitational field exerted by this mass would be strong enough to hold back light, and for it ...
... with the mass of the earth would have Rs ∼ 9mm! What this means is that we would have to cram the entire mass of the earth into a region of diameter less than 18mm (just over the size of a dime) before the gravitational field exerted by this mass would be strong enough to hold back light, and for it ...
Giant star seismology
... Asteroseismology – the study of global properties of stars and their internal structure through their global intrinsic oscillations – is already more than a century old. An early remarkable result was obtained for Cepheids revealing the period-luminosity relation (Leavitt and Pickering, 1912), which ...
... Asteroseismology – the study of global properties of stars and their internal structure through their global intrinsic oscillations – is already more than a century old. An early remarkable result was obtained for Cepheids revealing the period-luminosity relation (Leavitt and Pickering, 1912), which ...
Astronomical Circumstances
... This DRAFT document is an excerpt from Principles of Planetary Biology, by Tom E. Morris. based on their brightness (magnitude), temperature, receive each moment, so the warmer the planet will get radius, luminosity, mix of colors (spectral class), and (all other things being equal). This being the ...
... This DRAFT document is an excerpt from Principles of Planetary Biology, by Tom E. Morris. based on their brightness (magnitude), temperature, receive each moment, so the warmer the planet will get radius, luminosity, mix of colors (spectral class), and (all other things being equal). This being the ...
A Digital Spectral Classification Atlas
... Figure 11: The spectra of three helium-weak B-type stars compared with two MK standards. Spectra adapted from the Paranal Observatory spectral library, from the Indo-US coudé-feed library and from DSO. The star, 3 Sco, is an excellent example of a helium-weak B-type star. The hydrogen lines of this ...
... Figure 11: The spectra of three helium-weak B-type stars compared with two MK standards. Spectra adapted from the Paranal Observatory spectral library, from the Indo-US coudé-feed library and from DSO. The star, 3 Sco, is an excellent example of a helium-weak B-type star. The hydrogen lines of this ...
Influence of the Gould Belt on Interstellar Extinction
... objects, and the extinction for a typical large region of space can be determined as, say, 5.0m ± 0.5m , i.e., with an accuracy of 10%. An analytical model of extinction within the nearest kiloparsec with a relative accuracy higher than that of the model by Arenou et al. (1992) is unlikely to be po ...
... objects, and the extinction for a typical large region of space can be determined as, say, 5.0m ± 0.5m , i.e., with an accuracy of 10%. An analytical model of extinction within the nearest kiloparsec with a relative accuracy higher than that of the model by Arenou et al. (1992) is unlikely to be po ...