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... The Sun’s Atmosphere Even at a great distance from the Sun, you and your spacecraft can feel slight effects from the solar wind—the stream of charged particles continually blown outward in all directions from the Sun. Recall that the solar wind helps shape the magnetospheres of planets (see Figure 7 ...
... The Sun’s Atmosphere Even at a great distance from the Sun, you and your spacecraft can feel slight effects from the solar wind—the stream of charged particles continually blown outward in all directions from the Sun. Recall that the solar wind helps shape the magnetospheres of planets (see Figure 7 ...
Timescales for the evolution of oxygen isotope compositions in the
... We review two models for the origin of the calcium-, aluminum-rich inclusion (CAI) oxygen isotope mixing line in the solar nebula: (1) CO self-shielding, and (2) chemical mass-independent fractionation (MIF). We consider the timescales associated with formation of an isotopically anomalous water res ...
... We review two models for the origin of the calcium-, aluminum-rich inclusion (CAI) oxygen isotope mixing line in the solar nebula: (1) CO self-shielding, and (2) chemical mass-independent fractionation (MIF). We consider the timescales associated with formation of an isotopically anomalous water res ...
Search for an exosphere around 51 Pegasi B with ISO
... HD 168443 (G5) and HD 114762 (F9V). None of the stars have been observed to have photometric variations compatible with planetary eclipses. Only recently a transit event has been observed in HD209458 (G0V) (Henry et al. 1999). Evolution models predict that the planetary companions are able to surviv ...
... HD 168443 (G5) and HD 114762 (F9V). None of the stars have been observed to have photometric variations compatible with planetary eclipses. Only recently a transit event has been observed in HD209458 (G0V) (Henry et al. 1999). Evolution models predict that the planetary companions are able to surviv ...
PH607lec08
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
Extrasolar Planet Studies:The Italian Contribution
... abundance of the parent star Detailed LTE analysis of a set of Fe I and Fe II lines yields Teff=5850±50 K, log g=4.4±0.1, and [Fe/H]=−0.15±0.10. New method to derive mass and radius of the star: M⋆ = 0.980±0.062 Mo R⋆=1.000±0.034 Ro Age = 5.1±2.5 Gyr Mp=1.198±0.053 MJ Rp=1.220±0.044 RJ, TrES-2 is ...
... abundance of the parent star Detailed LTE analysis of a set of Fe I and Fe II lines yields Teff=5850±50 K, log g=4.4±0.1, and [Fe/H]=−0.15±0.10. New method to derive mass and radius of the star: M⋆ = 0.980±0.062 Mo R⋆=1.000±0.034 Ro Age = 5.1±2.5 Gyr Mp=1.198±0.053 MJ Rp=1.220±0.044 RJ, TrES-2 is ...
Chemical analysis of 24 dusty (pre-) main
... Despite the broad wavelength coverage, for several program stars only a few lines turned out to be appropriate for detailed abundance analyses. Such a circumstance is not unusual for A/B-type stars, where the condition that spectral lines with equivalent widths higher than 150 mÅ should be avoided i ...
... Despite the broad wavelength coverage, for several program stars only a few lines turned out to be appropriate for detailed abundance analyses. Such a circumstance is not unusual for A/B-type stars, where the condition that spectral lines with equivalent widths higher than 150 mÅ should be avoided i ...
3. What are the intrinsic and extrinsic environments of exoplanets?
... habitable exoplanets. We will identify stars that lack critical observations and, where possible, acquire the appropriate data through supplementary observations. In particular, the PU coronagraphic optics group is developing high-contrast imaging techniques that will be invaluable in identifying fa ...
... habitable exoplanets. We will identify stars that lack critical observations and, where possible, acquire the appropriate data through supplementary observations. In particular, the PU coronagraphic optics group is developing high-contrast imaging techniques that will be invaluable in identifying fa ...
IMCCE - Observer pages
... compared to others or to be reduced: most of the parameters needed for the reduction are provided in a specific wavelength corresponding to a standard filter. With large telescopes, the infra red observations may be very interesting: the bright giant planets become dark in some infra red wavelengths ...
... compared to others or to be reduced: most of the parameters needed for the reduction are provided in a specific wavelength corresponding to a standard filter. With large telescopes, the infra red observations may be very interesting: the bright giant planets become dark in some infra red wavelengths ...
ALMA Science Results
... • Cinthya Herrera, National Astronomical Observatory of Japan – Galaxy interations are key components of galaxy formation and evolution. Most of star formation occurs in very compact (few pc) massive (>10^5 Msun) super star clusters. What triggers their formation? – Cycle 2 data could not see SiO bu ...
... • Cinthya Herrera, National Astronomical Observatory of Japan – Galaxy interations are key components of galaxy formation and evolution. Most of star formation occurs in very compact (few pc) massive (>10^5 Msun) super star clusters. What triggers their formation? – Cycle 2 data could not see SiO bu ...
The Habitability of Proxima Centauri b I: Evolutionary Scenarios
... and NLTE effects, which make it extraordinarily difficult to identify elemental abundances; hence its composition is far more difficult to measure than for G and K dwarfs like α Cen A and B (Johnson & Apps 2009). Recently, Hinkel & Kane (2013) completed a reanalysis of published compositional studie ...
... and NLTE effects, which make it extraordinarily difficult to identify elemental abundances; hence its composition is far more difficult to measure than for G and K dwarfs like α Cen A and B (Johnson & Apps 2009). Recently, Hinkel & Kane (2013) completed a reanalysis of published compositional studie ...
Pulsed Accretion in the Young Binary &
... Type I variations are periodic in VRI bands and are caused by rotational modulation of the star with an asymmetric distribution of cold spots (due to strong magnetic fields) on the stellar surface. These are thought to be analogous to sunspots, although they can cover up to 40% of the stellar surfac ...
... Type I variations are periodic in VRI bands and are caused by rotational modulation of the star with an asymmetric distribution of cold spots (due to strong magnetic fields) on the stellar surface. These are thought to be analogous to sunspots, although they can cover up to 40% of the stellar surfac ...
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... who introduced the morphological classification scheme for galaxies still in use today. His “tuning fork” diagram (figure 1) differentiates ellipticals from unbarred and barred spirals, further classified according to the tightness and fine structure of their spiral arms which appears to correlate w ...
... who introduced the morphological classification scheme for galaxies still in use today. His “tuning fork” diagram (figure 1) differentiates ellipticals from unbarred and barred spirals, further classified according to the tightness and fine structure of their spiral arms which appears to correlate w ...
The Formation and Evolution of Massive Black Holes - Ira-Inaf
... produce a very massive star of up to a few thousand M⊙ before the first supernovae explode. When heavy elements are still rare, just about when the second generation of stars occurs, the final fate of a very massive star is to collapse into a black hole with a mass similar to that of its progenitor. ...
... produce a very massive star of up to a few thousand M⊙ before the first supernovae explode. When heavy elements are still rare, just about when the second generation of stars occurs, the final fate of a very massive star is to collapse into a black hole with a mass similar to that of its progenitor. ...
Seminar Outburst of Comet 17P/Holmes
... of November. By the beginning of January 1893 the comet was barely seen with telescope. Another outburst in brightness occured around Jan. 16 and the comet again became visible to the naked eye. After that the comet steadily faded and it’s final observations were reported in the beginning of April. ...
... of November. By the beginning of January 1893 the comet was barely seen with telescope. Another outburst in brightness occured around Jan. 16 and the comet again became visible to the naked eye. After that the comet steadily faded and it’s final observations were reported in the beginning of April. ...
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... & Luu 1993, review by Weissman 1995). A disk of comets/icy asteroids, also known as the Kuiper belt, contains tens of thousands of sizable bodies (> ∼100km diameter) and ∼109 small comets, and extends between 40 AU and ∼103 AU from the Sun. These new developments are giving a new perspective to our ...
... & Luu 1993, review by Weissman 1995). A disk of comets/icy asteroids, also known as the Kuiper belt, contains tens of thousands of sizable bodies (> ∼100km diameter) and ∼109 small comets, and extends between 40 AU and ∼103 AU from the Sun. These new developments are giving a new perspective to our ...
FIRST STELLAR ABUNDANCES IN THE DWARF IRREGULAR
... Unfortunately, most dIrr systems are too distant for the detailed study and abundance analyses of e.g. their red giant branch (RGB) stars, which are of great importance due to their large spread in age. Hence, to date few details on the chemical evolution of the dIrr galaxies have been available. In ...
... Unfortunately, most dIrr systems are too distant for the detailed study and abundance analyses of e.g. their red giant branch (RGB) stars, which are of great importance due to their large spread in age. Hence, to date few details on the chemical evolution of the dIrr galaxies have been available. In ...
Heavy Element Abundances in Late-B and Early
... Unfortunately, the results from IUE data are constrained by their limited signal-to-noise ratio (S/ N ) (seldom more than 40:1 even for the very best co-added data) and limited resolution (k=k 12000). For a small number of CP stars, observations made with the Hubble Space Telescope’s Goddard High ...
... Unfortunately, the results from IUE data are constrained by their limited signal-to-noise ratio (S/ N ) (seldom more than 40:1 even for the very best co-added data) and limited resolution (k=k 12000). For a small number of CP stars, observations made with the Hubble Space Telescope’s Goddard High ...
The physics of star formation
... is of central importance in astrophysics to understand how stars form and what determines their properties. The generally accepted view that stars form by the gravitational condensation of diffuse matter in space is very old, indeed almost as old as the concept of universal gravitational attraction ...
... is of central importance in astrophysics to understand how stars form and what determines their properties. The generally accepted view that stars form by the gravitational condensation of diffuse matter in space is very old, indeed almost as old as the concept of universal gravitational attraction ...
The cosmic origin of fluorine and sulphur
... small white dwarf in the middle of the picture, and around it the elements the giant star has produced and expelled into its surroundings are clearly visible. In practice my result means that all the fluorine we come in contact with, including that in our toothpaste, likely has been formed like this ...
... small white dwarf in the middle of the picture, and around it the elements the giant star has produced and expelled into its surroundings are clearly visible. In practice my result means that all the fluorine we come in contact with, including that in our toothpaste, likely has been formed like this ...
Aquarius (constellation)
Aquarius is a constellation of the zodiac, situated between Capricornus and Pisces. Its name is Latin for ""water-carrier"" or ""cup-carrier"", and its symbol is 20px (Unicode ♒), a representation of water.Aquarius is one of the oldest of the recognized constellations along the zodiac (the sun's apparent path). It was one of the 48 constellations listed by the 2nd century AD astronomer Ptolemy, and it remains one of the 88 modern constellations. It is found in a region often called the Sea due to its profusion of constellations with watery associations such as Cetus the whale, Pisces the fish, and Eridanus the river.