![Formation and stability of planetary orbits in binary systems](http://s1.studyres.com/store/data/015821804_1-e281aaa246c6a7ddd303c0cace646739-300x300.png)
Formation and stability of planetary orbits in binary systems
... occurrence of planet formation in binary systems is well supported (Patience et al 2002, Eggenberger et al. 2004 & 2007 and others). However, these planets have all formed in wide binaries, with orbital distances in the range of 20AU . The IM Pegasi system, however, is a very close binary, with an o ...
... occurrence of planet formation in binary systems is well supported (Patience et al 2002, Eggenberger et al. 2004 & 2007 and others). However, these planets have all formed in wide binaries, with orbital distances in the range of 20AU . The IM Pegasi system, however, is a very close binary, with an o ...
An atlas of 2.4 to 4.1 mu m ISO/SWS spectra of early - UvA-DARE
... In this paper, we present and study 75 spectra of early-type stars, 67 [2.4–4.1 µm] ISO/SWS spectra and 8 [3.5–4.1 µm] spectra observed with the United Kingdom Infrared Telescope (UKIRT). This sample includes OB, Be, and Luminous Blue Variable (LBV) stars. We discuss line trends as a function of spe ...
... In this paper, we present and study 75 spectra of early-type stars, 67 [2.4–4.1 µm] ISO/SWS spectra and 8 [3.5–4.1 µm] spectra observed with the United Kingdom Infrared Telescope (UKIRT). This sample includes OB, Be, and Luminous Blue Variable (LBV) stars. We discuss line trends as a function of spe ...
Article PDF - IOPscience
... (LR) and high-resolution (HR) modes (Houck et al. 2004). The short-high (SH) and long-high (LH) modules operate at 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 spa ...
... (LR) and high-resolution (HR) modes (Houck et al. 2004). The short-high (SH) and long-high (LH) modules operate at 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 spa ...
talk at lensing and dark matter conference Ohio state 2004
... The number of non-Macho events is predicted to be much smaller than the 13-17 events observed (using standard LMC and Milky Way stellar populations.) ...
... The number of non-Macho events is predicted to be much smaller than the 13-17 events observed (using standard LMC and Milky Way stellar populations.) ...
Chapter 17. Creating New Domains
... to create another Galaxy. Usually, all the Stars of a Galaxy are from the same Domain but it is possible to connect Stars of one domain to a Galaxy of another domain using a WormHole. A Universe is a complete executable system. A Universe can be either a single Galaxy or a collection of disconnected ...
... to create another Galaxy. Usually, all the Stars of a Galaxy are from the same Domain but it is possible to connect Stars of one domain to a Galaxy of another domain using a WormHole. A Universe is a complete executable system. A Universe can be either a single Galaxy or a collection of disconnected ...
Stellar Population Effects on the Inferred Photon Density at
... for the initial mass function (IMF) in our standard models, with a slope of -1.3 between 0.1 and 0.5 M and -2.35 at masses above this, extending to 100 M for the models used in this study. The shallow slope below a stellar mass of 0.5 M biases our models towards the more massive stellar populatio ...
... for the initial mass function (IMF) in our standard models, with a slope of -1.3 between 0.1 and 0.5 M and -2.35 at masses above this, extending to 100 M for the models used in this study. The shallow slope below a stellar mass of 0.5 M biases our models towards the more massive stellar populatio ...
Jaká kritéria jsou vhodná ke klasifikaci hvězd horní části hlavní
... spectra is one of the main tasks of astrophysics. Let it be stars, nebulae or galaxies that we observe, spectroscopy always gives us some useful information, that furthers our understanding of physics of the observed object. Spectroscopic methods are of great importance especially when it comes to c ...
... spectra is one of the main tasks of astrophysics. Let it be stars, nebulae or galaxies that we observe, spectroscopy always gives us some useful information, that furthers our understanding of physics of the observed object. Spectroscopic methods are of great importance especially when it comes to c ...
A New Assessment of Dark Matter in the Milky Way Galaxy
... within an exponential disc as compared to the peak velocity within the corresponding spherically distributed body is higher only by approximately 15 percent, while the velocities at large radii dier by only a negligible amount. Furthermore, the galaxy has more of a spherical character than that of ...
... within an exponential disc as compared to the peak velocity within the corresponding spherically distributed body is higher only by approximately 15 percent, while the velocities at large radii dier by only a negligible amount. Furthermore, the galaxy has more of a spherical character than that of ...
galaxy formation and evolution - Yale Astronomy
... progressively larger ones, possibly in a hierarchical fashion; the galaxies that we now observe may then just represent the smallest structures that have survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial den ...
... progressively larger ones, possibly in a hierarchical fashion; the galaxies that we now observe may then just represent the smallest structures that have survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial den ...
probing quasar environments with tunable filter
... AGN may be categorised in a variety of ways; a simple taxonomy is shown in table 1.1, in which they are classified according to two parameters: radio-loudness and the width of their emission lines. Sometimes, more than one class of object shares a given radio categorisation and optical type: these a ...
... AGN may be categorised in a variety of ways; a simple taxonomy is shown in table 1.1, in which they are classified according to two parameters: radio-loudness and the width of their emission lines. Sometimes, more than one class of object shares a given radio categorisation and optical type: these a ...
the Ëg infrared search for extraterrestrial civilizations with large
... 1.4. Scope and Purpose of this Paper As an essential step in our waste heat search, we have produced a clean catalog of the reddest sources resolved by WISE. The purpose of our focus, in this work, on resolved sources is twofold: resolved sources present their own challenges of interpretation and ph ...
... 1.4. Scope and Purpose of this Paper As an essential step in our waste heat search, we have produced a clean catalog of the reddest sources resolved by WISE. The purpose of our focus, in this work, on resolved sources is twofold: resolved sources present their own challenges of interpretation and ph ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... factor ∼2, while surprisingly the stellar mass density of the blue cloud has remained ...
... factor ∼2, while surprisingly the stellar mass density of the blue cloud has remained ...
Annual Report 2006/2007
... Galaxies contain billions of stars, as well as interstellar gas and dust, and are embedded in dark halos of unknown constitution. Astronomers are able to look back in time, by observing galaxies at ever greater distances. Because light travels at finite velocity, distant objects are seen at a time w ...
... Galaxies contain billions of stars, as well as interstellar gas and dust, and are embedded in dark halos of unknown constitution. Astronomers are able to look back in time, by observing galaxies at ever greater distances. Because light travels at finite velocity, distant objects are seen at a time w ...
Session 1: Stellar winds, diagnostics across the electromagnetic
... seven very luminous WNL stars is found in the Large Magellanic Cloud, disregarding all objects with indications of binarity. In the Small Magellanic Cloud (SMC) the fraction of confirmed binaries is high. We analyzed the composite WN+O spectra as such and obtained very high luminosities for the WN c ...
... seven very luminous WNL stars is found in the Large Magellanic Cloud, disregarding all objects with indications of binarity. In the Small Magellanic Cloud (SMC) the fraction of confirmed binaries is high. We analyzed the composite WN+O spectra as such and obtained very high luminosities for the WN c ...
Cosmological Constraints from the Virial Mass
... In this thesis, I present a new determination of the cluster mass function in a volume 107 h -3 Mpc3 using the ROSAT-2MASS-FAST Group Survey (R2FGS). R2FGS is an X-ray-selected sample of systems from the ROSAT All-Sky Survey in the region 6 > 0' and 0.01 < z < 0.06, with target galaxies for each sys ...
... In this thesis, I present a new determination of the cluster mass function in a volume 107 h -3 Mpc3 using the ROSAT-2MASS-FAST Group Survey (R2FGS). R2FGS is an X-ray-selected sample of systems from the ROSAT All-Sky Survey in the region 6 > 0' and 0.01 < z < 0.06, with target galaxies for each sys ...
MUFASA: The assembly of the red sequence
... In this work, we examine the red sequence in the Mufasa suite of cosmological hydrodynamic simulations. Mufasa produces one of the most data-concordant representations of the galaxy population across cosmic time among current galaxy formation models, in terms of global galaxy stellar (Davé, Thompso ...
... In this work, we examine the red sequence in the Mufasa suite of cosmological hydrodynamic simulations. Mufasa produces one of the most data-concordant representations of the galaxy population across cosmic time among current galaxy formation models, in terms of global galaxy stellar (Davé, Thompso ...
- Haverford Scholarship
... 2011) or luminosity distances of Type Ia supernovae (e.g., Hicken et al. 2009). The potential of cluster surveys as a cosmological probe has recently been demonstrated through the analysis of large X-ray and optically selected cluster samples spanning a wide range in redshift (e.g., Vikhlinin et al. ...
... 2011) or luminosity distances of Type Ia supernovae (e.g., Hicken et al. 2009). The potential of cluster surveys as a cosmological probe has recently been demonstrated through the analysis of large X-ray and optically selected cluster samples spanning a wide range in redshift (e.g., Vikhlinin et al. ...
KIC 8462852 Faded Throughout the Kepler Mission
... comparing its aperture photometry to the aperture photometry recorded from the calibrator stars, weighted by the signal to noise ratio of each of the calibration stars. We use the standard deviation of the flux measured among all observations recorded on that particular pixel as the uncertainty asso ...
... comparing its aperture photometry to the aperture photometry recorded from the calibrator stars, weighted by the signal to noise ratio of each of the calibration stars. We use the standard deviation of the flux measured among all observations recorded on that particular pixel as the uncertainty asso ...
The Westerbork Hydrogen Accretion in LOcal GAlaxieS \(HALOGAS
... SFR values in Col. (12), see below for details. The UGC IDs of the four targets which have been observed in the pilot survey described in this paper are indicated with a bold font. The galaxy parameters listed in Table 1 are taken from Tully (1988), except for vrot , which is from HyperLEDA (Paturel ...
... SFR values in Col. (12), see below for details. The UGC IDs of the four targets which have been observed in the pilot survey described in this paper are indicated with a bold font. The galaxy parameters listed in Table 1 are taken from Tully (1988), except for vrot , which is from HyperLEDA (Paturel ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... equivalent of US$100-$200, and it’s often possible to find a used pair for much less. Binoculars are ideal for beginning stargazers because they are intuitive to use and show a wide area of sky at one time. And they bring into view hundreds of deep-sky objects and thousands of stars that cannot be s ...
... equivalent of US$100-$200, and it’s often possible to find a used pair for much less. Binoculars are ideal for beginning stargazers because they are intuitive to use and show a wide area of sky at one time. And they bring into view hundreds of deep-sky objects and thousands of stars that cannot be s ...
Runaway collisions in young star clusters – II. Numerical results
... with α = 2.35, M min = 0.2 M and M max = 120 M . For this stellar population, the average mass is M∗ 0.69 M . There is no initial mass segregation. To investigate the role of the initial concentration of the cluster, we consider King models with W0 = 3 or 8 (Binney & Tremaine 1987, Section 4 ...
... with α = 2.35, M min = 0.2 M and M max = 120 M . For this stellar population, the average mass is M∗ 0.69 M . There is no initial mass segregation. To investigate the role of the initial concentration of the cluster, we consider King models with W0 = 3 or 8 (Binney & Tremaine 1987, Section 4 ...
Evidence of the accelerated expansion of the Universe from weak
... Finally, because it is a geometric effect, gravitational lensing depends on the source redshift distribution, where most earlier measurements have had to rely on external redshift calibrations from the small Hubble Deep Fields. Here, the impact of sampling variance was demonstrated by Benjamin et al. ...
... Finally, because it is a geometric effect, gravitational lensing depends on the source redshift distribution, where most earlier measurements have had to rely on external redshift calibrations from the small Hubble Deep Fields. Here, the impact of sampling variance was demonstrated by Benjamin et al. ...
The eccentricities of the barium stars
... Paulus (1993). The sample of barium stars includes both `mild' and `strong' according to the classification system devised by Warner (1965). Warner's classification scheme for the barium Ê line strength to indicate stars uses an estimate of the Ba ii 4554-A the extent of abundance anomalies on a sca ...
... Paulus (1993). The sample of barium stars includes both `mild' and `strong' according to the classification system devised by Warner (1965). Warner's classification scheme for the barium Ê line strength to indicate stars uses an estimate of the Ba ii 4554-A the extent of abundance anomalies on a sca ...
chemical compositions of rv tauri stars and related objects
... like spectral energy distributions (SEDs) and chemical composition but mainly from the viewing angle onto the disk. In this scenario the RVa objects are thought to be the ones with low inclination while objects with high inclination such that the disk is seen edge-on would appear as RVbs. Preston et ...
... like spectral energy distributions (SEDs) and chemical composition but mainly from the viewing angle onto the disk. In this scenario the RVa objects are thought to be the ones with low inclination while objects with high inclination such that the disk is seen edge-on would appear as RVbs. Preston et ...
Ages of young stars
... Although possible in only a few clusters, the LDB method is well-placed to calibrate other age estimation techniques used in those same clusters. Its usefulness in estimating ages for individual stars is limited; the detection of (undepleted) Li in a low-mass star at a known distance and luminosity, ...
... Although possible in only a few clusters, the LDB method is well-placed to calibrate other age estimation techniques used in those same clusters. Its usefulness in estimating ages for individual stars is limited; the detection of (undepleted) Li in a low-mass star at a known distance and luminosity, ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.