Using photometric analysis to determine characteristics of the V
... The main purpose of the experiment as described above is to characterize the newly found nova V‐2491 in the Cygnus constellation as show in figure 2. In order to do so, frames of that particular nova need to be taken over several nights and then analyze as a collecti ...
... The main purpose of the experiment as described above is to characterize the newly found nova V‐2491 in the Cygnus constellation as show in figure 2. In order to do so, frames of that particular nova need to be taken over several nights and then analyze as a collecti ...
134-Notes-a
... The cones in your eyes respond more to color, but depend on having bright light, whereas the rods behave well in low light, but do not detect colors. Thus, galaxies and nebulae (low-light objects) typically will appear as black and white objects to human eyes, even when viewed through a telescope. N ...
... The cones in your eyes respond more to color, but depend on having bright light, whereas the rods behave well in low light, but do not detect colors. Thus, galaxies and nebulae (low-light objects) typically will appear as black and white objects to human eyes, even when viewed through a telescope. N ...
Globular Clusters
... to internal and external dynamical interactions, they represent an ideal workbench to study STELLAR DYNAMICS and to test most exquisite theoretical dynamical models. If studied as a global system, GCs constitute fossil tracers of the dynamical and chemical evolution of the parent galaxy and can be u ...
... to internal and external dynamical interactions, they represent an ideal workbench to study STELLAR DYNAMICS and to test most exquisite theoretical dynamical models. If studied as a global system, GCs constitute fossil tracers of the dynamical and chemical evolution of the parent galaxy and can be u ...
The Circumstellar Medium of Massive Stars in Motion
... formation and evolution of Betelgeuse’s bow shock, using a modified version of the hydrodynamics code GADGET211 . We simulated RSGs moving at velocities ranging from 28 to 73 km s−1 through a uniform ISM. Results from two simulations are shown in Fig. (2), showing bow shocks at two different velocit ...
... formation and evolution of Betelgeuse’s bow shock, using a modified version of the hydrodynamics code GADGET211 . We simulated RSGs moving at velocities ranging from 28 to 73 km s−1 through a uniform ISM. Results from two simulations are shown in Fig. (2), showing bow shocks at two different velocit ...
Galaxies have different sizes and shapes.
... The disk of the Milky Way measures The Milky Way is about 100,000 light-years in diameter. more than 100,000 light-years in diameter. The bulge of densely packed stars at the center is located about 26,000 light-years from the Sun. A large but very faint layer of stars surrounds the disk and bulge. ...
... The disk of the Milky Way measures The Milky Way is about 100,000 light-years in diameter. more than 100,000 light-years in diameter. The bulge of densely packed stars at the center is located about 26,000 light-years from the Sun. A large but very faint layer of stars surrounds the disk and bulge. ...
1 Introduction - High Point University
... Table 6: Fill in the empty fields above. 3. Check show luminosity classes and show isoradius lines (if they are not already checked). The green region (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of al ...
... Table 6: Fill in the empty fields above. 3. Check show luminosity classes and show isoradius lines (if they are not already checked). The green region (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of al ...
s-process
... -2.1, when low-mass AGB stars begin to contribute from double shell burning. The s-process then dominates Ba production. The origin of heavy metals at the lowest Galactic metallicity ([Fe/H] = -4) is still not understood, but may be dominated by the weak s-process, or by a separate r-process in mass ...
... -2.1, when low-mass AGB stars begin to contribute from double shell burning. The s-process then dominates Ba production. The origin of heavy metals at the lowest Galactic metallicity ([Fe/H] = -4) is still not understood, but may be dominated by the weak s-process, or by a separate r-process in mass ...
Determining Distances to Other Galaxies
... If stars in the disk of a spiral galaxy are on slightly eccentric orbits, and the position angle of these ellipses vary with radius, a spiral-shaped density wave can be formed from a set of nested ovals. Density wave theory is really based on the premise that mutual gravitational attraction of stars ...
... If stars in the disk of a spiral galaxy are on slightly eccentric orbits, and the position angle of these ellipses vary with radius, a spiral-shaped density wave can be formed from a set of nested ovals. Density wave theory is really based on the premise that mutual gravitational attraction of stars ...
Preface 1 PDF
... can be inferred. Thanks to helioseismology, we know that the Sun rotates as a solid body in the radiative interior and that the convective envelope rotates differentially, with a shear layer in between. Such a shear is thought to be one of the ways in which the large-scale magnetic field of the Sun c ...
... can be inferred. Thanks to helioseismology, we know that the Sun rotates as a solid body in the radiative interior and that the convective envelope rotates differentially, with a shear layer in between. Such a shear is thought to be one of the ways in which the large-scale magnetic field of the Sun c ...
Is the central binary system of the planetary nebula Henize 2
... interestingly, in the study by Weidmann and Gamen (2011) there are several PNe that show a wide He II 5412 Å absorption line with a weak emission feature in the center of the wide absorption line. This forms a spectral structure similar to that of Henize 2–428. The most noticeable examples of this ...
... interestingly, in the study by Weidmann and Gamen (2011) there are several PNe that show a wide He II 5412 Å absorption line with a weak emission feature in the center of the wide absorption line. This forms a spectral structure similar to that of Henize 2–428. The most noticeable examples of this ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... and by means of X-rays fluxes, luminosities and plasma temperatures from XMM-Newton observations. The X-ray part of SOXS is composed by 7 XMM-Newton observations to which we have added 3 archive pointings. The maps below are the RGB mosaics of X-ray images of EPIC on board XMM-Newton and IR images o ...
... and by means of X-rays fluxes, luminosities and plasma temperatures from XMM-Newton observations. The X-ray part of SOXS is composed by 7 XMM-Newton observations to which we have added 3 archive pointings. The maps below are the RGB mosaics of X-ray images of EPIC on board XMM-Newton and IR images o ...
![Gugus Bintang [Compatibility Mode]](http://s1.studyres.com/store/data/007745973_1-cdf92b37339f4354c66eef546bd46492-300x300.png)
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.