Lecture 2 Abundances
... • Elements with differences greater than 25% (Table 5, Lodders 2009) are W (2.76), Ag (0.52), Cl (1.79), Rb(1.64), Ga (0.61), Au(1.54). Tl (1.43), Hf (1.43), and F (1.32). Some, like Au, Hf, Mn, and W have uncertain oscillator strengths and problems with line blending. Others, like Cl, Ga, and Rb ar ...
... • Elements with differences greater than 25% (Table 5, Lodders 2009) are W (2.76), Ag (0.52), Cl (1.79), Rb(1.64), Ga (0.61), Au(1.54). Tl (1.43), Hf (1.43), and F (1.32). Some, like Au, Hf, Mn, and W have uncertain oscillator strengths and problems with line blending. Others, like Cl, Ga, and Rb ar ...
Chapter 5 Summary
... The granulation of the photosphere is produced by convection currents of gas rising from below. ...
... The granulation of the photosphere is produced by convection currents of gas rising from below. ...
Lecture 10: Interstellar gas
... • On the other hand, once the spins in a hydrogen atom have become aligned, about 10 million years, on the average, pass before the proton flips and the atom drops to its lowest energy state. It emits a 21 cm photon. This is a rare event for any one atom. But because so many hydrogen atoms exist in ...
... • On the other hand, once the spins in a hydrogen atom have become aligned, about 10 million years, on the average, pass before the proton flips and the atom drops to its lowest energy state. It emits a 21 cm photon. This is a rare event for any one atom. But because so many hydrogen atoms exist in ...
stars-notes
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
common constellations
... nebula. If you get a pair of binoculars and look closely at this "star", you will see not one, but many stars. This is a sight that is easy for anyone to see, even without a telescope. If you have a telescope, you will be able to make out some of the giant cloud of gas that makes up this nebula. Thi ...
... nebula. If you get a pair of binoculars and look closely at this "star", you will see not one, but many stars. This is a sight that is easy for anyone to see, even without a telescope. If you have a telescope, you will be able to make out some of the giant cloud of gas that makes up this nebula. Thi ...
The Physics of Neutron Stars
... An examination of the Fermi energy of the particles (using equation 4) shows that it is 97 MeV. This is around 10% of the neutron rest mass, so we are still in the non-relativistic regime. The correction for ignoring relativity when computing the Fermi energy is of the order of a few percent. As see ...
... An examination of the Fermi energy of the particles (using equation 4) shows that it is 97 MeV. This is around 10% of the neutron rest mass, so we are still in the non-relativistic regime. The correction for ignoring relativity when computing the Fermi energy is of the order of a few percent. As see ...
HIGH RESOLTION SPH SIMULATIONS OF GALAXY CLUSTERS
... Very small dependence of UV flux. UV-heating not able to suppress small galaxies: Problem for semianalitical models to explain substructure in the ...
... Very small dependence of UV flux. UV-heating not able to suppress small galaxies: Problem for semianalitical models to explain substructure in the ...
Definitions of Magnitudes and Surface Brightness
... The quantity ------- has the physical units of W m – 2 and in galaxy studies is often represented in solar luminosities per square parsec and is given the symbol Σ - and is also called surface brightness. The reason for this definition lies in the origin of the magnitude system. For a given patch of ...
... The quantity ------- has the physical units of W m – 2 and in galaxy studies is often represented in solar luminosities per square parsec and is given the symbol Σ - and is also called surface brightness. The reason for this definition lies in the origin of the magnitude system. For a given patch of ...
High-Speed Ballistic Stellar Interlopers
... indicates that the stars are traveling fast with respect to their surroundings—roughly five times faster than typical young stars. The interlopers were most likely ejected from massive star clusters. Assuming their youthful phase lasts only a million years and they are traveling 100,000 miles per ho ...
... indicates that the stars are traveling fast with respect to their surroundings—roughly five times faster than typical young stars. The interlopers were most likely ejected from massive star clusters. Assuming their youthful phase lasts only a million years and they are traveling 100,000 miles per ho ...
Pulsating variable stars and the Hertzsprung
... Delta Scuti variables are a well-known type of pulsating variable belonging to the main sequence. This type of stars is notable for a very short period, lasts for hours. Typically, periods are in the range of 0.02-0.4 days. Brightness varies between 0.02m and ...
... Delta Scuti variables are a well-known type of pulsating variable belonging to the main sequence. This type of stars is notable for a very short period, lasts for hours. Typically, periods are in the range of 0.02-0.4 days. Brightness varies between 0.02m and ...
astronomy
... Discuss the nature of electromagnetic radiation, and tell how that radiation transfers energy and information through interstellar space. List the major regions of the electromagnetic spectrum and explain how the properties of the Earth’s atmosphere affect our ability to make astronomical observatio ...
... Discuss the nature of electromagnetic radiation, and tell how that radiation transfers energy and information through interstellar space. List the major regions of the electromagnetic spectrum and explain how the properties of the Earth’s atmosphere affect our ability to make astronomical observatio ...
Is there life in space? Activity 2: Moving Stars and Their Planets
... Q. Most of the planets that have been discovered orbit their stars at a tilt closer to 0 degrees than to 90 degrees. Why? A. The signal is more evident when the tilt is lower. The telescopes are not perfect, so they can only detect star motions that are very large. The largest motions occur when the ...
... Q. Most of the planets that have been discovered orbit their stars at a tilt closer to 0 degrees than to 90 degrees. Why? A. The signal is more evident when the tilt is lower. The telescopes are not perfect, so they can only detect star motions that are very large. The largest motions occur when the ...
Chapter 13 section 2
... absolute magnitude is about average. The Sun shines with a yellow light. Although the Sun is an average star, it is much closer to Earth than other stars. Light from the Sun reaches Earth in about eight minutes. Light from other stars takes many years to reach Earth. The Sun is unusual in one way. I ...
... absolute magnitude is about average. The Sun shines with a yellow light. Although the Sun is an average star, it is much closer to Earth than other stars. Light from the Sun reaches Earth in about eight minutes. Light from other stars takes many years to reach Earth. The Sun is unusual in one way. I ...
1 pracovni list HR diagram I EN
... Open the prepared CSV file in an Excel spreadsheet. To construct a H–R diagram you need to know the star’s luminosity (or absolute magnitude) and effective temperature (or spectral type or colour index). From the catalogue it is possible to obtain the absolute magnitude (calculated in column M from ...
... Open the prepared CSV file in an Excel spreadsheet. To construct a H–R diagram you need to know the star’s luminosity (or absolute magnitude) and effective temperature (or spectral type or colour index). From the catalogue it is possible to obtain the absolute magnitude (calculated in column M from ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.