Diapositiva 1
... main-sequence A stars because of our inability to distinguish marginal Am stars from normal ones in A2-F0 and our inability to disentangle evolutionary effects ...
... main-sequence A stars because of our inability to distinguish marginal Am stars from normal ones in A2-F0 and our inability to disentangle evolutionary effects ...
–1– 2. Milky Way We know a great deal, perhaps more than any
... • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is about 10 kpc, and the MW is flattened with an axial ratio of 1/5. The Sun is abo ...
... • A similar, but much larger survey of nearby stars was done by Kapteyn around 1920. He used parallax, proper motions, radial velocities and spectra to infer the distance to stars. He inferred that the size of the MW is about 10 kpc, and the MW is flattened with an axial ratio of 1/5. The Sun is abo ...
SEEING STARS! SEEING STARS!
... Print a copy of the Plough/Big Dipper Map (see end of activity sheet), and stick the map onto the piece of black cardboard. Poke a hole through where the stars appear on the paper (to transfer the map to the black card). Using the chart above measure a length of straw for each of the stars. Stick th ...
... Print a copy of the Plough/Big Dipper Map (see end of activity sheet), and stick the map onto the piece of black cardboard. Poke a hole through where the stars appear on the paper (to transfer the map to the black card). Using the chart above measure a length of straw for each of the stars. Stick th ...
X-ray Binaries in Nearby Galaxies
... Point, variable on short time scale X-ray sources Neutron Stars or Black Holes Accreting from binary companions ...
... Point, variable on short time scale X-ray sources Neutron Stars or Black Holes Accreting from binary companions ...
Calculating Radial Velocities of Low Mass Eclipsing Binaries
... occur during the eclipse of each system, and this was observed in almost every case. Notable exceptions include EBLM11 and EBLM19, whose radial velocities did not vary over time. It remains unclear why, but we can speculate that these were perhaps ...
... occur during the eclipse of each system, and this was observed in almost every case. Notable exceptions include EBLM11 and EBLM19, whose radial velocities did not vary over time. It remains unclear why, but we can speculate that these were perhaps ...
Red Dwarf Stars: Ages, Rotation, Magnetic
... pre-main sequence stars and close binaries in the sample. Also in this study, we exclude spectral types later than ∼M7 because they appear to have Age-Rotation-Activity relations quite different to earlier spectral types. From a limited sample of M7–9 V stars, it appears that they do not undergo mag ...
... pre-main sequence stars and close binaries in the sample. Also in this study, we exclude spectral types later than ∼M7 because they appear to have Age-Rotation-Activity relations quite different to earlier spectral types. From a limited sample of M7–9 V stars, it appears that they do not undergo mag ...
Think about the universe
... objects in the sky with much greater precision than ever before. Observations using telescopes showed that many different types of objects in the sky could be identified. These included single or double stars, groups of stars called galaxies, clusters of galaxies, and clouds of gas and dust called n ...
... objects in the sky with much greater precision than ever before. Observations using telescopes showed that many different types of objects in the sky could be identified. These included single or double stars, groups of stars called galaxies, clusters of galaxies, and clouds of gas and dust called n ...
The Circumstellar Medium of Massive Stars in Motion
... Massive stars are the main drivers of the evolution of the gaseous component of galaxies. They emit huge quantities of far-ultraviolet photons that ionise and heat surrounding gas; their strong winds drive shocks and gas flows; and their final explosions as supernovae or gamma-ray bursts generate po ...
... Massive stars are the main drivers of the evolution of the gaseous component of galaxies. They emit huge quantities of far-ultraviolet photons that ionise and heat surrounding gas; their strong winds drive shocks and gas flows; and their final explosions as supernovae or gamma-ray bursts generate po ...
The Spectra ot Novae
... a n d for a b o u t half of these, at least one s p e c t r o g r a m has been obtained. The record can be called extensive for fifteen stars. This material appears sufficient to j u s t i f y a t t e m p t s at generalization on such m a t t e r s as the typical course of d e v e l o p m e n t and ...
... a n d for a b o u t half of these, at least one s p e c t r o g r a m has been obtained. The record can be called extensive for fifteen stars. This material appears sufficient to j u s t i f y a t t e m p t s at generalization on such m a t t e r s as the typical course of d e v e l o p m e n t and ...
The old globular cluster system of the dIrr galaxy NGC 1427A in the
... Chile. In addition, near-infrared (NIR) images in J-band (1.5 µm) were taken with the Infrared Spectrometer And Array Camera (ISAAC) attached to the UT1 of the ESO/VLT. The complete NIR data set includes H and Ks imaging, however only the J-band was deep enough to perform this study. The FORS1 instr ...
... Chile. In addition, near-infrared (NIR) images in J-band (1.5 µm) were taken with the Infrared Spectrometer And Array Camera (ISAAC) attached to the UT1 of the ESO/VLT. The complete NIR data set includes H and Ks imaging, however only the J-band was deep enough to perform this study. The FORS1 instr ...
Lecture Notes – Galaxies
... Galaxies were first systematically categorized by Edwin Hubble who in 1929 classified them according to shape: the Hubble Classification Scheme or Tuning Fork Diagram Elliptical galaxies (‘Early type’) E0 – E7 (0 spherical, 7 most distorted): S0 These galaxies are intermediate between E0 and Sa – th ...
... Galaxies were first systematically categorized by Edwin Hubble who in 1929 classified them according to shape: the Hubble Classification Scheme or Tuning Fork Diagram Elliptical galaxies (‘Early type’) E0 – E7 (0 spherical, 7 most distorted): S0 These galaxies are intermediate between E0 and Sa – th ...
Star-D_Teacher_Guide - The University of Texas at Dallas
... * A white dwarf is a very small, hot star that is no longer on the main sequence ...
... * A white dwarf is a very small, hot star that is no longer on the main sequence ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Supernovae are not alike. For decades, astronomers had known that supernovae fell into different types based on their light curves, that is, their pattern of rising and falling brightness. Later, they found these types actually corresponded to different physical circumstances triggering the explosio ...
... Supernovae are not alike. For decades, astronomers had known that supernovae fell into different types based on their light curves, that is, their pattern of rising and falling brightness. Later, they found these types actually corresponded to different physical circumstances triggering the explosio ...
10 Measuring The Stars
... These stars are all more luminous than the Sun. Two new categories appear here – the red giants and the blue giants. Clearly, the brightest stars in the sky appear bright because of their enormous luminosities, not their ...
... These stars are all more luminous than the Sun. Two new categories appear here – the red giants and the blue giants. Clearly, the brightest stars in the sky appear bright because of their enormous luminosities, not their ...
Carbon Stars - The OzSky Star Safari
... area of the HR diagram that we call an 'instability strip' or an 'instability region'. When the star is in this area of the diagram it will become a variable star, one that varies in brightness over time.“ • “Mira stars are red giants (which began as low mass stars), with a temperature less than ...
... area of the HR diagram that we call an 'instability strip' or an 'instability region'. When the star is in this area of the diagram it will become a variable star, one that varies in brightness over time.“ • “Mira stars are red giants (which began as low mass stars), with a temperature less than ...
The Prospective Aspect of the Cosmogonic Models in Laozi and T
... momentum being less than of its surrounding planets and of the sun originating before the planets. – It was harshly attacked by Safronov, who felt that time needed for a thin cloud envelope to develop into planets would exceed the age of the solar system. ...
... momentum being less than of its surrounding planets and of the sun originating before the planets. – It was harshly attacked by Safronov, who felt that time needed for a thin cloud envelope to develop into planets would exceed the age of the solar system. ...
A Spectroscopic Study of the RV Tauri Stars TT Oph... Guillermo Hernandez , Donald K. Walter , Jennifer Cash
... RV Tauri stars are a small class of pulsating, luminous, yellow supergiants whose light curves are characterized by alternating deep and shallow minima. The time from one deep minima to the next deep minima is known as the formal period, while the time from one deep minima to the next shallow minima ...
... RV Tauri stars are a small class of pulsating, luminous, yellow supergiants whose light curves are characterized by alternating deep and shallow minima. The time from one deep minima to the next deep minima is known as the formal period, while the time from one deep minima to the next shallow minima ...
16. Magnitude Systems
... 1.Consider the star PG1633+099A, the discussion on how to convert between UBVRI and SDSS ugriz, and the SDSS DR8 Navigate Tool, all linked from the syllabus • use the UBVRI to ugriz transformations to show that the g magnitude displayed for PG1633+099A in the SDSS DR8 Navigate Tool is near the expec ...
... 1.Consider the star PG1633+099A, the discussion on how to convert between UBVRI and SDSS ugriz, and the SDSS DR8 Navigate Tool, all linked from the syllabus • use the UBVRI to ugriz transformations to show that the g magnitude displayed for PG1633+099A in the SDSS DR8 Navigate Tool is near the expec ...
An Eclectic View of our Milky Way Galaxy
... latter may be associated with the Hubble flow, while the former are clearly influenced by the gravitational influence of M31. An independent solution for the local circular velocity was derived by Reid et al. [42] using the positions, parallaxes, and proper motions of Galactic radio masers in conjun ...
... latter may be associated with the Hubble flow, while the former are clearly influenced by the gravitational influence of M31. An independent solution for the local circular velocity was derived by Reid et al. [42] using the positions, parallaxes, and proper motions of Galactic radio masers in conjun ...
Life Stages of High
... • After core helium fusion stops, He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer. • This double-shell-burning stage never reaches equilibrium—the fusion rate periodically spikes upward in a series of thermal pulses. • With each spike, con ...
... • After core helium fusion stops, He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer. • This double-shell-burning stage never reaches equilibrium—the fusion rate periodically spikes upward in a series of thermal pulses. • With each spike, con ...
00 T Tauri Stars Have Extensive Coronae?
... band, the corresponding scaling factor is less than 1,000. One explanation for this behaviour is that T Tauri stars have coronae wh ich are 104 to 106 times as strong as the solar corona, but most X-rays are absorbed in circumstellar gas which does not contribute to the visual extinction towards the ...
... band, the corresponding scaling factor is less than 1,000. One explanation for this behaviour is that T Tauri stars have coronae wh ich are 104 to 106 times as strong as the solar corona, but most X-rays are absorbed in circumstellar gas which does not contribute to the visual extinction towards the ...
8.2Apply Exponent Properties Involving Quotients
... 51. SPACE TRAVEL Alpha Centauri is the closest star system to Earth. Alpha ...
... 51. SPACE TRAVEL Alpha Centauri is the closest star system to Earth. Alpha ...
Solar-like oscillations in intermediate red giants
... There are modes with inertia similar to that of a radial modes. In principle, this modes might be excited to an observable level throught stochastic ...
... There are modes with inertia similar to that of a radial modes. In principle, this modes might be excited to an observable level throught stochastic ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.