Script Chapter 2, part 1
... Some examples for measured RV-curves for extra-solar planetary systems are shown in some of the accompanying slides: 51 Peg b: The historical detection measurements for 51 Peg b, the first extra-solar planets around a normal star, from Mayor and Queloz. The orbital period is about 4.2 days and the R ...
... Some examples for measured RV-curves for extra-solar planetary systems are shown in some of the accompanying slides: 51 Peg b: The historical detection measurements for 51 Peg b, the first extra-solar planets around a normal star, from Mayor and Queloz. The orbital period is about 4.2 days and the R ...
Labeling the HR Diagram - Mastering Physics Answers
... We can use the inverse square law for light to calculate the star’s luminosity from its apparent brightness and distance. However, this calculated value will be accurate only if there is no absorption or scattering of the light on its way from the star to us. (If there is interstellar dust between u ...
... We can use the inverse square law for light to calculate the star’s luminosity from its apparent brightness and distance. However, this calculated value will be accurate only if there is no absorption or scattering of the light on its way from the star to us. (If there is interstellar dust between u ...
Document
... 1) Target list with an idea of distances that do not exceed what is possible with your detector ...
... 1) Target list with an idea of distances that do not exceed what is possible with your detector ...
DISCOVERY OF HOT SUPERGIANT STARS NEAR THE GALACTIC
... Chandra X-Ray Observatory catalog of point sources in the Radio Arches region. Following up with K-band spectroscopy, we found two massive stellar counterparts to CXOGC J174555.3285126 and CXOGC J174617.0285131, which we classify as a broad-lined WR star of subtype WN6b and an O Ia supergiant, res ...
... Chandra X-Ray Observatory catalog of point sources in the Radio Arches region. Following up with K-band spectroscopy, we found two massive stellar counterparts to CXOGC J174555.3285126 and CXOGC J174617.0285131, which we classify as a broad-lined WR star of subtype WN6b and an O Ia supergiant, res ...
Archaeoastronomical Study of the Main Pyramids of Giza
... As reported above, an additional anti-clockwise rotation of 15.3˚ is required to overlap the Orion Belt stars on the corresponding pyramids. Actually, such a rotation is necessary since the “axis of the Pyramids” (i.e. the straight line that best fits the positions of the centers, or vertexes, of th ...
... As reported above, an additional anti-clockwise rotation of 15.3˚ is required to overlap the Orion Belt stars on the corresponding pyramids. Actually, such a rotation is necessary since the “axis of the Pyramids” (i.e. the straight line that best fits the positions of the centers, or vertexes, of th ...
Stellar Evolution - Astrophysics
... ing angular fiducials is to use background reference stars are infinitely distant, the parallactic angle as it tained from the two sub-frames of Fig. 1 readily p sired angular measure. However, since the backgro in fact not infinitely distant, they themselves march (albeit smaller) parallactic motio ...
... ing angular fiducials is to use background reference stars are infinitely distant, the parallactic angle as it tained from the two sub-frames of Fig. 1 readily p sired angular measure. However, since the backgro in fact not infinitely distant, they themselves march (albeit smaller) parallactic motio ...
Article PDF - IOPscience
... The vast majority of Kepler stars are in a distance range of roughly 200–1000 pc relative to the solar system (corresponding to a diffraction-limited separation of 10–50 AU at WIYN, and 4–20 AU at Gemini North). The range of Galactic latitude and longitude appropriate for the Kepler field is 5.◦ 5 ...
... The vast majority of Kepler stars are in a distance range of roughly 200–1000 pc relative to the solar system (corresponding to a diffraction-limited separation of 10–50 AU at WIYN, and 4–20 AU at Gemini North). The range of Galactic latitude and longitude appropriate for the Kepler field is 5.◦ 5 ...
Lokal fulltext - Chalmers Publication Library
... of mass m (Salpeter, 1955). This means that low-mass stars are significantly more numerous than high-mass stars. For example, there are about 225 times as many solar-mass (1 M ) stars as there are stars of mass 10 M . Mass is an important factor in determining the properties of stars, along with t ...
... of mass m (Salpeter, 1955). This means that low-mass stars are significantly more numerous than high-mass stars. For example, there are about 225 times as many solar-mass (1 M ) stars as there are stars of mass 10 M . Mass is an important factor in determining the properties of stars, along with t ...
astro-ph/9505110 PDF
... Our results are shown in Figures 4 and 5 (Garnett et al. 1994, 1995). We nd that the C/O ratio increases monotonically as a function of O/H, from about 1/4 solar at the lowest metallicities up to solar values. At the same time, C/N also appears to increase with O/H in the irregular galaxies, but th ...
... Our results are shown in Figures 4 and 5 (Garnett et al. 1994, 1995). We nd that the C/O ratio increases monotonically as a function of O/H, from about 1/4 solar at the lowest metallicities up to solar values. At the same time, C/N also appears to increase with O/H in the irregular galaxies, but th ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
The P Cygni supergiant [OMN2000] LS1
... To derive the stellar parameters for [OMN2000] LS1 one must adopt a distance to it and, by extension, the W51 complex. Figueruedo et al. (2008) provides a summary of the results of previous studies. These show that the kinematic estimate of the distance - utilising radio recombination lines - of 5.5 ...
... To derive the stellar parameters for [OMN2000] LS1 one must adopt a distance to it and, by extension, the W51 complex. Figueruedo et al. (2008) provides a summary of the results of previous studies. These show that the kinematic estimate of the distance - utilising radio recombination lines - of 5.5 ...
LANL Cosmology Summer School Lectures, July 2010
... • Find: MH2 > 1010 Mo> Mstars => early stage of MWtype galaxy formation? • Again: low order CO is big (28kpc) • Milky Way-like CO excitation (low order key!) ...
... • Find: MH2 > 1010 Mo> Mstars => early stage of MWtype galaxy formation? • Again: low order CO is big (28kpc) • Milky Way-like CO excitation (low order key!) ...
The Milky Way as a galaxy
... the sphere. Like two railway tracks that run parallel but do not appear parallel to us, the vectors of proper motions in a star cluster also do not appear parallel. They are directed towards a convergence point, as depicted in Fig. 2.4. We shall demonstrate next how to use this effect to determine t ...
... the sphere. Like two railway tracks that run parallel but do not appear parallel to us, the vectors of proper motions in a star cluster also do not appear parallel. They are directed towards a convergence point, as depicted in Fig. 2.4. We shall demonstrate next how to use this effect to determine t ...
BREATHING IN LOW MASS GALAXIES: A STUDY - N
... Grebel & Harbeck 2003) or the shorter timescale fluctuations seen at the present day. However, there is growing evidence from dwarf spheroidal age-metallicity relations that gas accretion and outflows may have played a role, leading to G- and K-dwarf problems comparable to those seen in the Milky Wa ...
... Grebel & Harbeck 2003) or the shorter timescale fluctuations seen at the present day. However, there is growing evidence from dwarf spheroidal age-metallicity relations that gas accretion and outflows may have played a role, leading to G- and K-dwarf problems comparable to those seen in the Milky Wa ...
Search for giant planets in M67 III: excess of Hot Jupiters in dense
... surveys in the OCs M67, Hyades and Praesepe, we would determine a rate of 6/240 HJs/surveyed stars (including some binaries), that is huge when compared to 10/836 of the Wright et al. (2012) field sample. We can conclude that, contrary to early reports, the frequency of HJs discovered in the three O ...
... surveys in the OCs M67, Hyades and Praesepe, we would determine a rate of 6/240 HJs/surveyed stars (including some binaries), that is huge when compared to 10/836 of the Wright et al. (2012) field sample. We can conclude that, contrary to early reports, the frequency of HJs discovered in the three O ...
Lab 7
... 10. How many Sun-like stars (remember, even if it's in the same spectral class as the Sun, it can't be part of a multiple-star system — except under certain circumstances!) are there on this model? What percentage of all the stars in the model are Sun-like? ...
... 10. How many Sun-like stars (remember, even if it's in the same spectral class as the Sun, it can't be part of a multiple-star system — except under certain circumstances!) are there on this model? What percentage of all the stars in the model are Sun-like? ...
Massive quiescent galaxies at cosmic noon Robert Feldmann UC Berkeley
... • galaxy & halo growth are strongly correlated (similar timescales) • Low specific growth rates necessary to become quiescent ...
... • galaxy & halo growth are strongly correlated (similar timescales) • Low specific growth rates necessary to become quiescent ...
The deep OB star population in Carina from the VST Photometric Hα
... and how this should be tensioned against the possibility of forming massive stars outside densely clustered environments (de Wit et al. 2005; Bressert et al. 2012). Furthermore, as we await the arrival of advanced astrometry from ESA’s Gaia mission, it is the perfect time to trace how OB stars fit i ...
... and how this should be tensioned against the possibility of forming massive stars outside densely clustered environments (de Wit et al. 2005; Bressert et al. 2012). Furthermore, as we await the arrival of advanced astrometry from ESA’s Gaia mission, it is the perfect time to trace how OB stars fit i ...
Planetary Companions to Evolved Intermediate
... theories applicable to more massive stars than the Sun have begun to be developed rapidly (Ida & Lin 2005; Burkert & Ida 2007; Kennedy & Kenyon 2008) as an extension of the standard theory for solar-mass ones (e.g., Hayashi et al. 1985; Ida & Lin 2004) for the first time since Nakano (1988) explored ...
... theories applicable to more massive stars than the Sun have begun to be developed rapidly (Ida & Lin 2005; Burkert & Ida 2007; Kennedy & Kenyon 2008) as an extension of the standard theory for solar-mass ones (e.g., Hayashi et al. 1985; Ida & Lin 2004) for the first time since Nakano (1988) explored ...
Chapter 15 Stars, Galaxies, and Universe
... •One star brighter, more massive •Dimmer star’s gravity causes “wobble” •Eclipsing binary – one star blocks light from another star •Triple stars – 3 stars together •Found at least 500 other planets that revolve around stars- called exoplanets. •Found by “wobble” of star. ...
... •One star brighter, more massive •Dimmer star’s gravity causes “wobble” •Eclipsing binary – one star blocks light from another star •Triple stars – 3 stars together •Found at least 500 other planets that revolve around stars- called exoplanets. •Found by “wobble” of star. ...
Galaxy Number Counts from the Sloan Digital Sky Survey
... Photo examines every detected object for multiple peaks; if they exist, the object is deblended (Lupton et al. unpublished) into a hierarchy of component objects (children), and the parent is flagged as BLENDED. If a parent object has a large number of peaks, then only the 30 highest peaks are deble ...
... Photo examines every detected object for multiple peaks; if they exist, the object is deblended (Lupton et al. unpublished) into a hierarchy of component objects (children), and the parent is flagged as BLENDED. If a parent object has a large number of peaks, then only the 30 highest peaks are deble ...
Spiral galaxies - Ira-Inaf
... H2 masses in the inner kpc region range from: 3 – 5 x 108 to >109 Msun. The extraordinary case of NGC 1961 (Combes+ 2009) has M(H2)~2x1010 Msun. M(dyn) ~ RV2/G. M(H2)/M(dyn) from a few percent up to > 20%. This means that more than 1/5 of the mass in the central few kpc of a galaxy can be molecular ...
... H2 masses in the inner kpc region range from: 3 – 5 x 108 to >109 Msun. The extraordinary case of NGC 1961 (Combes+ 2009) has M(H2)~2x1010 Msun. M(dyn) ~ RV2/G. M(H2)/M(dyn) from a few percent up to > 20%. This means that more than 1/5 of the mass in the central few kpc of a galaxy can be molecular ...
Development of a Fourier Technique for Automated Spiral Galaxy
... very important for performing surface photometry. In the B-band, the surface brightness of the outer regions of a typical nearby galaxy is fainter than that of the night sky by about 5 mag/arcsec2 , which corresponds to a factor of 100 in flux. Thus, extreme care must be taken to precisely compute t ...
... very important for performing surface photometry. In the B-band, the surface brightness of the outer regions of a typical nearby galaxy is fainter than that of the night sky by about 5 mag/arcsec2 , which corresponds to a factor of 100 in flux. Thus, extreme care must be taken to precisely compute t ...
Building galaxies Hunt, Leslie Kipp
... conjectured that “There may be innumerable spheres of this kind or starry heavens in the finite universe”. Thomas Wright of Durham, England, a few years after, interpreted the observations at that time of “the many cloudy Spots, just perceivable by us, as far without our starry Regions”. This idea w ...
... conjectured that “There may be innumerable spheres of this kind or starry heavens in the finite universe”. Thomas Wright of Durham, England, a few years after, interpreted the observations at that time of “the many cloudy Spots, just perceivable by us, as far without our starry Regions”. This idea w ...
1 Pau Amaro Seoane - modest 15-s
... We present an expression of the external gravitational field of a general ring-like object with the axial and plane symmetries such as annular disks or oval toroids with an arbitrary density distribution. The main term is that of an infinitely thin ring (Fukushima, 2010, Celest. Mech. Dyn. Astron., ...
... We present an expression of the external gravitational field of a general ring-like object with the axial and plane symmetries such as annular disks or oval toroids with an arbitrary density distribution. The main term is that of an infinitely thin ring (Fukushima, 2010, Celest. Mech. Dyn. Astron., ...
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.