story of telescope
... visions through every new telescope have changed our ideas about the universe. In the last century, scientists have even put telescopes in space to be able to observe the universe undeterred by the blanket of our atmosphere on Earth. They have also constructed telescopes to view the universe as it w ...
... visions through every new telescope have changed our ideas about the universe. In the last century, scientists have even put telescopes in space to be able to observe the universe undeterred by the blanket of our atmosphere on Earth. They have also constructed telescopes to view the universe as it w ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... describing these programs, and considering our radiative transfer models (see Sect. 3). Excluded sources include those with very poor S/N IRS data, sources where the SED and spectrum did not match at all (indicating that the IRS peak-up was on a source other than the intended target), sources with a ...
... describing these programs, and considering our radiative transfer models (see Sect. 3). Excluded sources include those with very poor S/N IRS data, sources where the SED and spectrum did not match at all (indicating that the IRS peak-up was on a source other than the intended target), sources with a ...
Ages of young stars
... These results show that LDB age uncertainties have yet to attain the floor set by levels of theoretical understanding. There is scope for improvement, particularly in defining the position of the LDB, photometric calibration of cool stars and better estimates of cluster distances. The LDB technique ...
... These results show that LDB age uncertainties have yet to attain the floor set by levels of theoretical understanding. There is scope for improvement, particularly in defining the position of the LDB, photometric calibration of cool stars and better estimates of cluster distances. The LDB technique ...
Ages of Young Stars
... These results show that LDB age uncertainties have yet to attain the floor set by levels of theoretical understanding. There is scope for improvement, particularly in defining the position of the LDB, photometric calibration of cool stars and better estimates of cluster distances. The LDB technique ...
... These results show that LDB age uncertainties have yet to attain the floor set by levels of theoretical understanding. There is scope for improvement, particularly in defining the position of the LDB, photometric calibration of cool stars and better estimates of cluster distances. The LDB technique ...
Downloaded - Royal Society Open Science
... All stars experience the ‘red giant branch’ (RGB) phase, when hydrogen in the core is exhausted and the remaining hydrogen burns in a contracting shell as the envelope expands. The extent of convection in the star increases, potentially ‘dredging-up’ already-burnt matter. Eventually, core temperatur ...
... All stars experience the ‘red giant branch’ (RGB) phase, when hydrogen in the core is exhausted and the remaining hydrogen burns in a contracting shell as the envelope expands. The extent of convection in the star increases, potentially ‘dredging-up’ already-burnt matter. Eventually, core temperatur ...
Diapositive 1
... • the sky (celestial sphere, constellations, light pollution) • the stars (stellar observables, H.-R. diagram) • the Pleiades (stellar parallaxes, stellar evolution, H.-R. diagram) • the Barnard’s star (proper motions) • confirmation of a candidate Supernova (astrometry, SN) • the shape of galaxies ...
... • the sky (celestial sphere, constellations, light pollution) • the stars (stellar observables, H.-R. diagram) • the Pleiades (stellar parallaxes, stellar evolution, H.-R. diagram) • the Barnard’s star (proper motions) • confirmation of a candidate Supernova (astrometry, SN) • the shape of galaxies ...
White dwarf binary
... Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as carbon white dwarfs Very low-mass stars with < 0.5MSun never become hot enough to fuse helium nuclei, and end as helium white ...
... Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as carbon white dwarfs Very low-mass stars with < 0.5MSun never become hot enough to fuse helium nuclei, and end as helium white ...
Here
... plus important iron group elements. These have been used to calculate the evolution of minor isotopes in TP-AGB stars of 1.5, 3 and 5 M at metallicities of Z = 0.02, 0.008 and 0.004 evolved with mass loss. The results of these calculations are compared to known constraints from spectroscopic observ ...
... plus important iron group elements. These have been used to calculate the evolution of minor isotopes in TP-AGB stars of 1.5, 3 and 5 M at metallicities of Z = 0.02, 0.008 and 0.004 evolved with mass loss. The results of these calculations are compared to known constraints from spectroscopic observ ...
PDF - ASSA
... pulsar wind nebulae, the final stages in the evolution of massive stars. There, charged particles are accelerated to extreme velocities. When these particles encounter light or gas in and around the cosmic accelerators, they emit gamma rays. Very high-energy gamma rays can be measured on Earth by obs ...
... pulsar wind nebulae, the final stages in the evolution of massive stars. There, charged particles are accelerated to extreme velocities. When these particles encounter light or gas in and around the cosmic accelerators, they emit gamma rays. Very high-energy gamma rays can be measured on Earth by obs ...
Multiplicity in Early Stellar Evolution
... with an eye toward determining cluster properties such as the initial mass function (e.g., Clark et al., 2008; Offner et al., 2009) and the number of brown dwarfs formed (e.g., Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). 3D HD SPH calculations by Bate (2009a) made predictions of the ...
... with an eye toward determining cluster properties such as the initial mass function (e.g., Clark et al., 2008; Offner et al., 2009) and the number of brown dwarfs formed (e.g., Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). 3D HD SPH calculations by Bate (2009a) made predictions of the ...
On the nature of sn stars. I. A detailed abundance study
... lower rotational velocity. However, the apparent preference of sn stars for objects with the lower vsini values should be taken with caution due to the small number of objects studied here. We analysed the photospheric chemical composition of sn stars and show that approximately ∼40% of them display ...
... lower rotational velocity. However, the apparent preference of sn stars for objects with the lower vsini values should be taken with caution due to the small number of objects studied here. We analysed the photospheric chemical composition of sn stars and show that approximately ∼40% of them display ...
Astronomy Astrophysics - Niels Bohr Institutet
... of groups of stars are intertwined with such easily observable properties as brightness, colours, and proper motions in ways that can make it difficult or impossible to retrieve the former from the latter. Kinematic selection biases are particularly pernicious in this regard. F- and G-type dwarf stars ...
... of groups of stars are intertwined with such easily observable properties as brightness, colours, and proper motions in ways that can make it difficult or impossible to retrieve the former from the latter. Kinematic selection biases are particularly pernicious in this regard. F- and G-type dwarf stars ...
About the Instructor`s Guide
... lead author changed his graduate study plans from biophysics to astrophysics as a result of watching the series.) Thus, while the series does not correspond directly to the textbook, it makes an outstanding resource for reinforcing key ideas. There are at least two basic ways in which you can use th ...
... lead author changed his graduate study plans from biophysics to astrophysics as a result of watching the series.) Thus, while the series does not correspond directly to the textbook, it makes an outstanding resource for reinforcing key ideas. There are at least two basic ways in which you can use th ...
Hubble Deep Field Academy -- Overview
... description, the concepts covered, prerequisites, and the target audience. Science Background: Provides information about the science behind the activity. It clarifies important concepts used in the activity and contains a message from the scientist who worked with the team to develop it. Lesson Pla ...
... description, the concepts covered, prerequisites, and the target audience. Science Background: Provides information about the science behind the activity. It clarifies important concepts used in the activity and contains a message from the scientist who worked with the team to develop it. Lesson Pla ...
The Role of Radioactive Isotopes in Astrophysics
... environmental situations in stars within which selected isotopes would be abundant, fleshing out ideas that Suess had envisioned earlier for two neutron-capture processes. Suess had, however, been unable to formulate these clearly enough to win contemporary acclaim. The slow neutron-capture process, ...
... environmental situations in stars within which selected isotopes would be abundant, fleshing out ideas that Suess had envisioned earlier for two neutron-capture processes. Suess had, however, been unable to formulate these clearly enough to win contemporary acclaim. The slow neutron-capture process, ...
GRB prompt emission
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
GRB prompt emission
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
April 2016 - Central Arkansas Astronomical Society
... composed of a pulsar in orbit around a neutron star. Taylor Louisiana, and Hanford, Washington, USA. The LIGO and Joel M. Weisberg in 1982 found that the orbit of the Observatories are funded by the Na onal Science pulsar was slowly shrinking over me because of the release Founda on (NSF), and were ...
... composed of a pulsar in orbit around a neutron star. Taylor Louisiana, and Hanford, Washington, USA. The LIGO and Joel M. Weisberg in 1982 found that the orbit of the Observatories are funded by the Na onal Science pulsar was slowly shrinking over me because of the release Founda on (NSF), and were ...
Article PDF - IOPscience
... a resolution of R ∼ 600 with wavelength coverage from 9.9 to 37.2 μm; the short-low (SL1 and SL2) and long-low (LL1 and LL2) modules operate at resolutions R ∼ 56–127, with coverage spanning 5.2–38 μm. There also exist two “bonus segments” that cover the overlapping range between the first and secon ...
... a resolution of R ∼ 600 with wavelength coverage from 9.9 to 37.2 μm; the short-low (SL1 and SL2) and long-low (LL1 and LL2) modules operate at resolutions R ∼ 56–127, with coverage spanning 5.2–38 μm. There also exist two “bonus segments” that cover the overlapping range between the first and secon ...
- StealthSkater
... table, stars in spectral class 'G' have stable lifespans of 10 billion years. (Our Sun -- actually a 'G2' star - has a somewhat longer stable life expectancy of 11 billion years.) We are about 5 billion years into that period, so we can look forward to the Sun remaining much as it is (actually it wi ...
... table, stars in spectral class 'G' have stable lifespans of 10 billion years. (Our Sun -- actually a 'G2' star - has a somewhat longer stable life expectancy of 11 billion years.) We are about 5 billion years into that period, so we can look forward to the Sun remaining much as it is (actually it wi ...