Forming Jupiter, Saturn, Uranus and Neptune in few million years by
... and n(m) is the number of bodies in a linear mass bin. For a constant value of a the R mass in the interval is nmdm / m2a . Depending on the value of a the mass in the interval would be mostly contained in small (a > 2) or large (a < 2) planetesimals. Wetherill and Stewart (1993) studied the evolut ...
... and n(m) is the number of bodies in a linear mass bin. For a constant value of a the R mass in the interval is nmdm / m2a . Depending on the value of a the mass in the interval would be mostly contained in small (a > 2) or large (a < 2) planetesimals. Wetherill and Stewart (1993) studied the evolut ...
A large-scale CO survey of the Rosette Molecular Cloud: assessing
... extended components were identified as ambient, relatively undisturbed cool gas clouds in the region (Heyer et al. 2006). In the following sections we investigate the first two types of compact structures in more detail. 3.1 High-velocity outflows Inspection of the full data cube reveal seven potent ...
... extended components were identified as ambient, relatively undisturbed cool gas clouds in the region (Heyer et al. 2006). In the following sections we investigate the first two types of compact structures in more detail. 3.1 High-velocity outflows Inspection of the full data cube reveal seven potent ...
Exploration of the Kuiper Belt by High-Precision Photometric
... KBOs down to objects of 1 km radius leads to 1011 KBOs with a total mass of only 0.1 Mo (Gladman et al. 2001). In contrast, a simple extrapolation of the surface mass density of the solar system outside 35 AU yields several Earth masses. Moreover, KBO accretion models require an initial Kuiper Belt ...
... KBOs down to objects of 1 km radius leads to 1011 KBOs with a total mass of only 0.1 Mo (Gladman et al. 2001). In contrast, a simple extrapolation of the surface mass density of the solar system outside 35 AU yields several Earth masses. Moreover, KBO accretion models require an initial Kuiper Belt ...
A star`s life is a struggle between ______ wanting to crush it, and
... evolved faster than the higher mass one. b) The red giant might be made of some different elements, so it evolved faster. c) The lower mass star used to be a more massive main sequence star, but when it became a giant some of its mass was transferred to the other star. ...
... evolved faster than the higher mass one. b) The red giant might be made of some different elements, so it evolved faster. c) The lower mass star used to be a more massive main sequence star, but when it became a giant some of its mass was transferred to the other star. ...
Essential Question
... 6. If a star has a low surface temperature and is considered very dim, where would you expect it to be located on the Herztsprung-Russell diagram? ...
... 6. If a star has a low surface temperature and is considered very dim, where would you expect it to be located on the Herztsprung-Russell diagram? ...
Hands-On Radio Astronomy Mapping the Milky Way
... like to be able to embark on a spaceship and see the Galaxy from outside. Unfortunately, traveling in and around the Galaxy is (and will always be) out of the question because of the huge distances. We are condemned to observe the Galaxy from the vicinity of the Sun. In addition, some areas of the M ...
... like to be able to embark on a spaceship and see the Galaxy from outside. Unfortunately, traveling in and around the Galaxy is (and will always be) out of the question because of the huge distances. We are condemned to observe the Galaxy from the vicinity of the Sun. In addition, some areas of the M ...
Summary - X-ray Astronomy Group at ISAS
... Narrow +broad Fe K lines are common- but not ubiquitous ionized Fe K lines detected -Chandra grating obs. Seyfert II galaxies are photoionization dominated--grating observations Majority of AGN in the universe do not have strong optical lines or bright optical nuclei– XMM and Chandra deep fields Ser ...
... Narrow +broad Fe K lines are common- but not ubiquitous ionized Fe K lines detected -Chandra grating obs. Seyfert II galaxies are photoionization dominated--grating observations Majority of AGN in the universe do not have strong optical lines or bright optical nuclei– XMM and Chandra deep fields Ser ...
Galactic Evolution - Harvard-Smithsonian Center for Astrophysics
... they must have been very much more massive than any stars existing today, hence very much shorter lived than any stars now known. Such pure gas, lacking in C and O that normally help clouds to cool and condense, would have needed more mass to contract than stars typically now, >10 Gy after the bang ...
... they must have been very much more massive than any stars existing today, hence very much shorter lived than any stars now known. Such pure gas, lacking in C and O that normally help clouds to cool and condense, would have needed more mass to contract than stars typically now, >10 Gy after the bang ...
Calculate the Mass of the Milky Way Galaxy
... • During the uncertainties of the era, Hubble was able to observe galaxies at distances up to 7 million light years away. By doing so he was able to come up with Hubble's Law, which said that the further galaxies were away from earth the faster they moved away from our planet. Hubble's rule proved t ...
... • During the uncertainties of the era, Hubble was able to observe galaxies at distances up to 7 million light years away. By doing so he was able to come up with Hubble's Law, which said that the further galaxies were away from earth the faster they moved away from our planet. Hubble's rule proved t ...
GAIA A Stereoscopic Census of our Galaxy
... - flush frequency: 15 MHz - readout frequency: 30 kHz - total read noise: 6e- rms ...
... - flush frequency: 15 MHz - readout frequency: 30 kHz - total read noise: 6e- rms ...
Galaxies
... IRREGULARS The final galaxy class identified by Hubble—irregular galaxies—named in this way because their visual appearance does not allow us to place them into any of the other categories just discussed. Irregulars tend to be rich in interstellar matter and young, blue stars, but they lack any regu ...
... IRREGULARS The final galaxy class identified by Hubble—irregular galaxies—named in this way because their visual appearance does not allow us to place them into any of the other categories just discussed. Irregulars tend to be rich in interstellar matter and young, blue stars, but they lack any regu ...
Understanding the Astrophysics of Galaxy Evolution: the role of
... correlated with dark matter halo mass and so the best link to the underlying cosmological model. A survey must be large (∼ few ×105 galaxies) in order to disentangle covariances in the physical properties of galaxies. One reason it is so difficult to understand how galaxies form is because almost al ...
... correlated with dark matter halo mass and so the best link to the underlying cosmological model. A survey must be large (∼ few ×105 galaxies) in order to disentangle covariances in the physical properties of galaxies. One reason it is so difficult to understand how galaxies form is because almost al ...
IXO as an observatory in the large telescopes era
... drive star formation and black hole growth (in proto-quasar active galaxies) until a luminous quasar forms. At this point, a black hole driven wind evacuates gas from the nascent galaxy, limiting additional star formation and further black hole growth (Silk & Rees 1998; Fig. 1). Further episodes of ...
... drive star formation and black hole growth (in proto-quasar active galaxies) until a luminous quasar forms. At this point, a black hole driven wind evacuates gas from the nascent galaxy, limiting additional star formation and further black hole growth (Silk & Rees 1998; Fig. 1). Further episodes of ...
スライド 1 - STScI
... shows the 10 sigma detection limit for our monitoring survey at K band, which is about 15.5 magnitude. The right diagonal line stands for the 10 sigma detection limit of the OGLE survey at I band, which is about 19.5 magnitude. Also, the left diagonal line shows the saturation limit of the OGLE surv ...
... shows the 10 sigma detection limit for our monitoring survey at K band, which is about 15.5 magnitude. The right diagonal line stands for the 10 sigma detection limit of the OGLE survey at I band, which is about 19.5 magnitude. Also, the left diagonal line shows the saturation limit of the OGLE surv ...
Age dating stellar populations in the near infrared
... versus the J−H (F110W–F160W) colour for the inner (top panel) and outer (bottom panel) fields of M83 (Bastian et al. 2011, 2012). These colours have not been dereddened. The solid red curve displays our theoretically calculated colour evolution using Geneva evolutionary tracks and colours calculated ...
... versus the J−H (F110W–F160W) colour for the inner (top panel) and outer (bottom panel) fields of M83 (Bastian et al. 2011, 2012). These colours have not been dereddened. The solid red curve displays our theoretically calculated colour evolution using Geneva evolutionary tracks and colours calculated ...
WASP-86b and WASP-102b: super-dense versus bloated planets
... just to mention a few, are capable of detecting peculiar objects for example HATS-17 b, (Penev et al. 2016); HATS-18 b, (Brahm et al. 2016), increasing the spectrum of possible massradius relations in the planetary regime. These systems provide invaluable observational constraints on theoretical mod ...
... just to mention a few, are capable of detecting peculiar objects for example HATS-17 b, (Penev et al. 2016); HATS-18 b, (Brahm et al. 2016), increasing the spectrum of possible massradius relations in the planetary regime. These systems provide invaluable observational constraints on theoretical mod ...
hwd_ewd_v3 - X-ray and Observational Astronomy Group
... The basis for understanding the nature of most stars is analysis of their optical spectra and classification according to the characteristics revealed. A number of physical processes can alter the atmospheric composition of a white dwarf as it cools. As noted by Schatzman4, the strong gravitational ...
... The basis for understanding the nature of most stars is analysis of their optical spectra and classification according to the characteristics revealed. A number of physical processes can alter the atmospheric composition of a white dwarf as it cools. As noted by Schatzman4, the strong gravitational ...
![arXiv:1606.05438v1 [astro-ph.SR] 17 Jun 2016](http://s1.studyres.com/store/data/013048193_1-92364881cbcc0fdb7f47e7990acc1537-300x300.png)
Chemical composition of cosmic dust in the solar vicinity
... The Cosmic Dust Analyser on the Cassini spacecraft has detected the faint but distinct signature of dust coming from outside our Solar System, from the local interstellar cloud. Altobelli et al. (2016): “It can be verified that Mg/Si, Fe/Si, Mg/Fe, and Ca/Fe ratios are on average CI chondritic (carb ...
... The Cosmic Dust Analyser on the Cassini spacecraft has detected the faint but distinct signature of dust coming from outside our Solar System, from the local interstellar cloud. Altobelli et al. (2016): “It can be verified that Mg/Si, Fe/Si, Mg/Fe, and Ca/Fe ratios are on average CI chondritic (carb ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.