Neistein_dekel60
... The history of one galaxy We follow all the particles, and check which got heated/cooled/SF/accreted ...
... The history of one galaxy We follow all the particles, and check which got heated/cooled/SF/accreted ...
Vibrational instability of Population III very massive mainsequence
... Accepted 2011 November 29. Received 2011 November 24; in original form 2011 October 11 ...
... Accepted 2011 November 29. Received 2011 November 24; in original form 2011 October 11 ...
Ultra-luminous Quasars with the Most Massive Black Holes at
... The first low-resolution optical spectrum of this source was obtained with the Lijiang 2.4 m telescope using the YFOSC on 2013 November 25 (UT), then follow-up by Magellan. ...
... The first low-resolution optical spectrum of this source was obtained with the Lijiang 2.4 m telescope using the YFOSC on 2013 November 25 (UT), then follow-up by Magellan. ...
Solar X-ray and UV radiation at Earth`s surface 4–3.5 billion years ago
... 1972]. This refers to the apparently paradoxical evidence for the presence of liquid water (as clearly indicated by geological evidence such as pillow basalts), while the Sun did not provide sufficient energy for water to be present at the Earth’s surface in any other form than ice, under presentday ...
... 1972]. This refers to the apparently paradoxical evidence for the presence of liquid water (as clearly indicated by geological evidence such as pillow basalts), while the Sun did not provide sufficient energy for water to be present at the Earth’s surface in any other form than ice, under presentday ...
Finding high-redshift dark stars with the James Webb Space
... Whether infalling WIMPs could restore the balance before the star evolves into a supernova or a black hole may depend on the overall structural evolution of the minihalo (e.g. contraction, mergers with other halos), on tidal interactions of the dark star with subhalos, gas clouds and possibly other ...
... Whether infalling WIMPs could restore the balance before the star evolves into a supernova or a black hole may depend on the overall structural evolution of the minihalo (e.g. contraction, mergers with other halos), on tidal interactions of the dark star with subhalos, gas clouds and possibly other ...
The Solar Nebula - Lincoln-Sudbury Regional High School
... The Solar System is made up of the Sun, nine planets, dozens of satellites, planetary ring systems, and thousands of asteroids and comets. The planets can be broken up into two distinct groups: the inner rocky terrestrials and the outer gaseous Jovians, plus Pluto, which fits into neither category. ...
... The Solar System is made up of the Sun, nine planets, dozens of satellites, planetary ring systems, and thousands of asteroids and comets. The planets can be broken up into two distinct groups: the inner rocky terrestrials and the outer gaseous Jovians, plus Pluto, which fits into neither category. ...
Search for giant planets in M67 - III. Excess of hot Jupiters in dense
... −2.6 % for single stars and 4.5%−2.5 % for the full sample). This rate is much higher than what has been discovered in the field, either with RV surveys or by transits. High metallicity is not a cause for the excess of HJs in M67, nor can the excess be attributed to high stellar masses. When combini ...
... −2.6 % for single stars and 4.5%−2.5 % for the full sample). This rate is much higher than what has been discovered in the field, either with RV surveys or by transits. High metallicity is not a cause for the excess of HJs in M67, nor can the excess be attributed to high stellar masses. When combini ...
O stars with weak winds: the Galactic case - Max-Planck
... the broader the profile, the lower the precision of the fit of the line. The typical error on Teff is usually of ± 2000 K but can be reduced when many optical He lines are available. Note that the errors we give are 2σ errors (we have Teff − error < Teff < Teff + error). We also checked that our fin ...
... the broader the profile, the lower the precision of the fit of the line. The typical error on Teff is usually of ± 2000 K but can be reduced when many optical He lines are available. Note that the errors we give are 2σ errors (we have Teff − error < Teff < Teff + error). We also checked that our fin ...
The radio structure of radio-quiet quasars
... the A, BnA, and B configuration at 4.8 GHz or 8.4 GHz with two intermediate frequencies (IFs) of 50 MHz bandwidth. The details of the observations are given in Table 1. The data reduction was performed in the typical manner using the Aips software. All bright sources were subject to several iteratio ...
... the A, BnA, and B configuration at 4.8 GHz or 8.4 GHz with two intermediate frequencies (IFs) of 50 MHz bandwidth. The details of the observations are given in Table 1. The data reduction was performed in the typical manner using the Aips software. All bright sources were subject to several iteratio ...
Atypical thermonuclear supernovae from tidally crushed white dwarfs
... where n∗ is the star density in the star cluster nucleus and Mh,3 is the hole’s mass in units of 103 M . This fiducial capture rate may need to be modified for a number of reasons. The actual rate could be lower than that given by equation (4), even if the initial distribution were isotropic, if the ...
... where n∗ is the star density in the star cluster nucleus and Mh,3 is the hole’s mass in units of 103 M . This fiducial capture rate may need to be modified for a number of reasons. The actual rate could be lower than that given by equation (4), even if the initial distribution were isotropic, if the ...
Multiwavelength Observations of Massive Stellar Cluster Candidates
... and the results were cross-correlated. If a source was not present in one or more of the 4.5, 5.8, ...
... and the results were cross-correlated. If a source was not present in one or more of the 4.5, 5.8, ...
Plasmonic waveguide filters with nanodisk resonators
... between the free electrons in a metal and the electromagnetic field in a dielectric, and attenuating exponentially in the direction perpendicular to the interface. [1] ...
... between the free electrons in a metal and the electromagnetic field in a dielectric, and attenuating exponentially in the direction perpendicular to the interface. [1] ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
The P Cygni supergiant [OMN2000] LS1
... OMN2000 described it as a ‘P Cygni type supergiant’ and classified it as O4 I, with a progenitor mass of ∼120M⊙ , making it of considerable interest as one of the most massive, evolved stars in the Galaxy. In this work we present new high resolution ...
... OMN2000 described it as a ‘P Cygni type supergiant’ and classified it as O4 I, with a progenitor mass of ∼120M⊙ , making it of considerable interest as one of the most massive, evolved stars in the Galaxy. In this work we present new high resolution ...
Plane Mirrors
... 1) A plane mirror produces a real / virtual (choose one) image. This is known as the image’s TYPE. 2) A plane mirror produces an upright / inverted (choose one) image. This is known as the image’s ATTITUDE. 3) A plane mirror produces a larger / smaller / same size (choose one) image. This is known a ...
... 1) A plane mirror produces a real / virtual (choose one) image. This is known as the image’s TYPE. 2) A plane mirror produces an upright / inverted (choose one) image. This is known as the image’s ATTITUDE. 3) A plane mirror produces a larger / smaller / same size (choose one) image. This is known a ...
5.3.2 Processing Light
... The incoming beam is polarized at 45o relative to the principal polarization directions in the anisotropic medium. The two beams exciting the medium produce a circular polarization as shown in the animation (© Wikipedia) How is it done? Let's look at the "old" and slightly modified picture above to ...
... The incoming beam is polarized at 45o relative to the principal polarization directions in the anisotropic medium. The two beams exciting the medium produce a circular polarization as shown in the animation (© Wikipedia) How is it done? Let's look at the "old" and slightly modified picture above to ...
幻灯片 1 - 长安大学精品课程网站
... The resulting patterns of light are a result of the wave nature of light and cannot be understood on the basis of rays. Optical effects that depend on the wave nature of light are grouped under the heading physical optics. In this chapter we'll look at interference phenomena that occur when two wav ...
... The resulting patterns of light are a result of the wave nature of light and cannot be understood on the basis of rays. Optical effects that depend on the wave nature of light are grouped under the heading physical optics. In this chapter we'll look at interference phenomena that occur when two wav ...
Pre-main sequence stars, emission stars and recent star formation in
... Myr), there is a chance for a spread in the age of the stars, depending on the duration of star formation. An estimation of this formation time-scale in the clusters formed in a star forming complex, will indicate the duration of star formation and its direction of propagation within the complex. In ...
... Myr), there is a chance for a spread in the age of the stars, depending on the duration of star formation. An estimation of this formation time-scale in the clusters formed in a star forming complex, will indicate the duration of star formation and its direction of propagation within the complex. In ...
Hertzsprung-Russell Diagram Outline
... From a star’s spectrum, we can determine its spectral and luminosity class. Given the star’s apparent brightness (observed flux), we can then estimate its distance. This distance determination technique is called spectroscopic ...
... From a star’s spectrum, we can determine its spectral and luminosity class. Given the star’s apparent brightness (observed flux), we can then estimate its distance. This distance determination technique is called spectroscopic ...
stellar interiors instructor notes
... 1. Develop the basic equations describing equilibrium conditions applying in stellar ...
... 1. Develop the basic equations describing equilibrium conditions applying in stellar ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.