Ch12&13 Life and Death of Stars
... • Things get interesting after about 9 billion years…. • A star remains on the main sequence as long as it can fuse hydrogen into helium in its core ...
... • Things get interesting after about 9 billion years…. • A star remains on the main sequence as long as it can fuse hydrogen into helium in its core ...
PODEX – PhOtometric Data EXtractor
... First, the bias image is subtracted from the raw image and the residual image is divided by the flat field image (optional). After these corrections the image is divided by integration time to normalise the intensity to ADU per second. A sub–image (the size is defined by the preference parameter cen ...
... First, the bias image is subtracted from the raw image and the residual image is divided by the flat field image (optional). After these corrections the image is divided by integration time to normalise the intensity to ADU per second. A sub–image (the size is defined by the preference parameter cen ...
12_Doppler (Mar 12)
... following statements best describes how the sources of light that produced the two spectra were moving? BLUE ...
... following statements best describes how the sources of light that produced the two spectra were moving? BLUE ...
Chapter 13 The Stellar Graveyard
... around 1.0 M⊙, its luminosity is very consistent, and can be used as a standard candle for the measurement of distance to distant galaxies (Chapter 15). The amount of energy produced by white dwarf supernovae and massive star supernovae are about the same. But the properties of the light emitted fro ...
... around 1.0 M⊙, its luminosity is very consistent, and can be used as a standard candle for the measurement of distance to distant galaxies (Chapter 15). The amount of energy produced by white dwarf supernovae and massive star supernovae are about the same. But the properties of the light emitted fro ...
Powerpoint - Physics and Astronomy
... As stars evolve during their main-sequence lifetime a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteristics of surfa ...
... As stars evolve during their main-sequence lifetime a) they gradually become cooler and dimmer (spectral type O to type M). b) they gradually become hotter and brighter (spectral type M to type O). c) they don’t change their spectral type. Explanation: A star’s main-sequence characteristics of surfa ...
Lecture 11
... – Hot gas in accretion disks can emit X-rays – The accretion disk can dump material which may become hot and dense enough to under nuclear fusion. • What is a white dwarf supernova – White dwarf accretes gas from companion until it exceeds 1.4 solar masses – which undergoes collapse and destruct ...
... – Hot gas in accretion disks can emit X-rays – The accretion disk can dump material which may become hot and dense enough to under nuclear fusion. • What is a white dwarf supernova – White dwarf accretes gas from companion until it exceeds 1.4 solar masses – which undergoes collapse and destruct ...
Unit 1
... A. Nuclear burning induced by the black hole B. Expansion of the Universe locally near the black hole C. Effect of the gravitational field on virtual electronpositron pairs arising due to the quantum mechanical ...
... A. Nuclear burning induced by the black hole B. Expansion of the Universe locally near the black hole C. Effect of the gravitational field on virtual electronpositron pairs arising due to the quantum mechanical ...
Chapter 23 The Milky Way Galaxy
... research was done by analysis of photographs; this work was mostly done by women (called “computers,” as they did computations). Several of these women went on to become well-known astronomers in their own right. Their work enabled the advances made by Shapley as well as Hertzsprung and Russell, amo ...
... research was done by analysis of photographs; this work was mostly done by women (called “computers,” as they did computations). Several of these women went on to become well-known astronomers in their own right. Their work enabled the advances made by Shapley as well as Hertzsprung and Russell, amo ...
Final Review Sheet
... 10**10 yr/(M/Msun)**2 The sun was less luminous in the past and will be more luminous in the future. Its radius is gradually increasing, but it is getting denser in its center. V. Post Main Sequence Evolution of Stars Lighter than 8 Msun Hydrogen fuel exhausted in inner 10 - 15% of mass. Helium core ...
... 10**10 yr/(M/Msun)**2 The sun was less luminous in the past and will be more luminous in the future. Its radius is gradually increasing, but it is getting denser in its center. V. Post Main Sequence Evolution of Stars Lighter than 8 Msun Hydrogen fuel exhausted in inner 10 - 15% of mass. Helium core ...
HIERARCHICAL GALAXY ASSEMBLY AND ITS MANIFESTATIONS
... Colour-colour relations at z~2: star-forming vs passive galaxies ...
... Colour-colour relations at z~2: star-forming vs passive galaxies ...
SGHS Faulkes ASISTM Star Cluster Photometry
... The colour of a star is due to the temperature of its outer atmosphere. Relatively cool stars are orange or red and hot stars are white or blue. The temperature of a star’s outer layers is determined by how much energy a star is giving out and how far the star’s outer layers are from the centre of t ...
... The colour of a star is due to the temperature of its outer atmosphere. Relatively cool stars are orange or red and hot stars are white or blue. The temperature of a star’s outer layers is determined by how much energy a star is giving out and how far the star’s outer layers are from the centre of t ...
Stellar Evolution
... What happens when a star, fusing hydrogen into helium on the main sequence, exhausts the hydrogen in the core? • hydrogen burning stops, star loses energy • core contracts, and gets hotter • higher temperature allows new nuclear reactions to start that are very slow at the ~15 million K temperature ...
... What happens when a star, fusing hydrogen into helium on the main sequence, exhausts the hydrogen in the core? • hydrogen burning stops, star loses energy • core contracts, and gets hotter • higher temperature allows new nuclear reactions to start that are very slow at the ~15 million K temperature ...
A Planetary System Around Our Nearest Star is Emerging
... The new planet, Alpha Centauri Bb (Alf Cen B b for short), orbits the secondary star Alpha Centauri B with a period at 0.04 the Earth-Sun distance from the star. A this short distance, the planet receives about 310 times more light than Earth receives from the Sun, making its surface very hot, nearl ...
... The new planet, Alpha Centauri Bb (Alf Cen B b for short), orbits the secondary star Alpha Centauri B with a period at 0.04 the Earth-Sun distance from the star. A this short distance, the planet receives about 310 times more light than Earth receives from the Sun, making its surface very hot, nearl ...
Gemini - Sochias
... 40-200 AU separation Second epoch observations of 48 stars confirm all candidates as unrelated background stars 95% upper limit of fractions of star with at least one planet of 0.5 - 13 MJup are – 0.28 for 10-25 AU – 0.13 for 25-50 AU ...
... 40-200 AU separation Second epoch observations of 48 stars confirm all candidates as unrelated background stars 95% upper limit of fractions of star with at least one planet of 0.5 - 13 MJup are – 0.28 for 10-25 AU – 0.13 for 25-50 AU ...
X-ray binaries
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
Extragalactic Astrophysics 1 AA 2011-2012 Prof. LA Antonelli
... subtracting solar motion, it is found that Milky Way and M31 approach each other at V~120 km/s most other galaxies have velocities within ~60 km/s from MilkyWay+M31 center of mass, not enough to escape from LG: Local Group represents a typical galactic environment: less dense than a galaxy cluster l ...
... subtracting solar motion, it is found that Milky Way and M31 approach each other at V~120 km/s most other galaxies have velocities within ~60 km/s from MilkyWay+M31 center of mass, not enough to escape from LG: Local Group represents a typical galactic environment: less dense than a galaxy cluster l ...
What units are used in astronomical photometry?
... Astrometry: Technological advances (including the Hubble Space Telescope) have improved parallax accuracy to 0.001” within a few years. Before 1990, fewer than 10,000 stellar parallaxes had been measured (and only 500 known well), but there are about 10 12 stars in our Galaxy. Space observations mad ...
... Astrometry: Technological advances (including the Hubble Space Telescope) have improved parallax accuracy to 0.001” within a few years. Before 1990, fewer than 10,000 stellar parallaxes had been measured (and only 500 known well), but there are about 10 12 stars in our Galaxy. Space observations mad ...
A Collection of Curricula for the STARLAB Deep Sky Objects
... Nebulae absorb light from nearby stars and radiate it back into space. Most nebulae glow red, the color of hydrogen gas. The brightest nebula is the Orion Nebula (see slide #60) which can be seen with the unaided eye in a dark sky. Nebulae are very important in astronomy because they are the key to ...
... Nebulae absorb light from nearby stars and radiate it back into space. Most nebulae glow red, the color of hydrogen gas. The brightest nebula is the Orion Nebula (see slide #60) which can be seen with the unaided eye in a dark sky. Nebulae are very important in astronomy because they are the key to ...
Study Guide for 1ST Astronomy Exam
... Describe in words and using the Whole Sky Map, developed in class, the annual motion of the Sun eastward through the stars along the ecliptic defining and identifying the special points on the ecliptic (solstices and equinoxes), Describe quantitatively the apparent daily motion of the Sun on an ...
... Describe in words and using the Whole Sky Map, developed in class, the annual motion of the Sun eastward through the stars along the ecliptic defining and identifying the special points on the ecliptic (solstices and equinoxes), Describe quantitatively the apparent daily motion of the Sun on an ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.