Document
... For stars like the sun, the oscillation period is 5 min → 1 min exposure time For good RV measurement you need S/N = 200 On a 2m telescope with a good spectrograph you can get S/N = 100 (10000 photons) in one hour on a V=10 star → 400.000 photons on a V=6 star in one hour, 6600 photons in one minute ...
... For stars like the sun, the oscillation period is 5 min → 1 min exposure time For good RV measurement you need S/N = 200 On a 2m telescope with a good spectrograph you can get S/N = 100 (10000 photons) in one hour on a V=10 star → 400.000 photons on a V=6 star in one hour, 6600 photons in one minute ...
I. Determination of stellar Parameters
... • Accuracy of distances of planet host stars increased substantially from ground-based (a) to Hipparcos (b). • Hipparcos provides proper motions for a large sample of stars and is a major step in the study of stellar streams. • … more to come with GAIA! ...
... • Accuracy of distances of planet host stars increased substantially from ground-based (a) to Hipparcos (b). • Hipparcos provides proper motions for a large sample of stars and is a major step in the study of stellar streams. • … more to come with GAIA! ...
3 Nightly Motions
... If a star is far enough to the north: It will not rise or set at all! Its path will simply carry it around the North Star in approximately 24 hours, always staying above the horizon. ...
... If a star is far enough to the north: It will not rise or set at all! Its path will simply carry it around the North Star in approximately 24 hours, always staying above the horizon. ...
Document
... “The presence of interstellar gas can be seen when you look at the spectral lines of a binary star system. Among the broad lines that shift as the two stars orbit each other, you see narrow lines that do not move. The narrow lines are from much colder gas in the interstellar medium between us and t ...
... “The presence of interstellar gas can be seen when you look at the spectral lines of a binary star system. Among the broad lines that shift as the two stars orbit each other, you see narrow lines that do not move. The narrow lines are from much colder gas in the interstellar medium between us and t ...
Engineering the Heavens
... error, whereas the German style was not just his care in the actual measurements. His sucsought precision by recognizing that error was always prescess also lay in his extraordinary rigor in spending five full ent and ever changing, so the astronomer must constantly years—1829 to 1834—calibrating th ...
... error, whereas the German style was not just his care in the actual measurements. His sucsought precision by recognizing that error was always prescess also lay in his extraordinary rigor in spending five full ent and ever changing, so the astronomer must constantly years—1829 to 1834—calibrating th ...
Tutorial: Motion
... If you get stuck or are not sure of your answer ask another group If you get really stuck or don’t understand what the Lecture Tutorial is asking as one of us for help ...
... If you get stuck or are not sure of your answer ask another group If you get really stuck or don’t understand what the Lecture Tutorial is asking as one of us for help ...
Tour of the Universe
... ● The planets that are farther away from the Sun are formed from cores of rock and metals and an abundance of ice. These planets include Jupiter, Saturn, Uranus and Neptune. These planets are called “Gas Giants” or “jovian”. ● Pluto is a dwarf planet. ● The planets move in an elliptical orbit. ...
... ● The planets that are farther away from the Sun are formed from cores of rock and metals and an abundance of ice. These planets include Jupiter, Saturn, Uranus and Neptune. These planets are called “Gas Giants” or “jovian”. ● Pluto is a dwarf planet. ● The planets move in an elliptical orbit. ...
Our_Unique_Planet
... “Magnetic Field” surrounding the earth. This provides protection from hard stellar radiation (ex. Solar Wind ) for us as well as keeping the atmosphere from being ...
... “Magnetic Field” surrounding the earth. This provides protection from hard stellar radiation (ex. Solar Wind ) for us as well as keeping the atmosphere from being ...
Doppler Effect - SAVE MY EXAMS!
... The initial discovery of the planet was made using the radial velocity method which involved measuring a Doppler shift in the spectrum of the star. Explain how an orbiting planet causes a Doppler shift in the spectrum of a star. ...
... The initial discovery of the planet was made using the radial velocity method which involved measuring a Doppler shift in the spectrum of the star. Explain how an orbiting planet causes a Doppler shift in the spectrum of a star. ...
Sama (Sky) | Questions on Islam
... The stars will gradually cool down and shrink because they get the energy to radiate from nucleus cohesions and thus losing their masses. Finally, as a result of shrinking, they will disperse because they will break free from the mutual gravitation force. Any two masses in the space attract each oth ...
... The stars will gradually cool down and shrink because they get the energy to radiate from nucleus cohesions and thus losing their masses. Finally, as a result of shrinking, they will disperse because they will break free from the mutual gravitation force. Any two masses in the space attract each oth ...
Lecture 1 – Astronomy
... • Large distances - unpractical to use km. • We use «light years» • Light travels 300 000 km per second. • How many km is a light-year? One light-year = 299 792 km/s x 60s x 60m x 24t x 365d = 9 460 000 000 000 km ...
... • Large distances - unpractical to use km. • We use «light years» • Light travels 300 000 km per second. • How many km is a light-year? One light-year = 299 792 km/s x 60s x 60m x 24t x 365d = 9 460 000 000 000 km ...
Lecture 2 - The University Centre in Svalbard
... • Large distances - unpractical to use km. • We use «light years» • Light travels 300 000 km per second. • How many km is a light-year? One light-year = 299 792 km/s x 60s x 60m x 24t x 365d = 9 460 000 000 000 km ...
... • Large distances - unpractical to use km. • We use «light years» • Light travels 300 000 km per second. • How many km is a light-year? One light-year = 299 792 km/s x 60s x 60m x 24t x 365d = 9 460 000 000 000 km ...
Unit 1
... core becomes too slow – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
... core becomes too slow – Radiation carries away energy in regions where the photons are not readily absorbed by stellar gas – Close to the cores of massive stars, there is enough material to impede the flow of energy through radiation ...
Phase Analysis of RV Tauri and Semi-regular Variables Abstract
... We examined the light curves of ten Semi-Regular or RV Tauri variable stars, related classes of pulsating variable stars. The ultimate objective for our research is to determine whether the stars stellar properties such as temperature, radius, and luminosity correlate with their pulsation cycles. In ...
... We examined the light curves of ten Semi-Regular or RV Tauri variable stars, related classes of pulsating variable stars. The ultimate objective for our research is to determine whether the stars stellar properties such as temperature, radius, and luminosity correlate with their pulsation cycles. In ...
File
... – what type of star it is, which give us… – its absolute brightness (among other things) • For example, the stars that are close enough to have their distance measured with parallax will have their spectrum analyzed. • From this, we can determine how bright a certain class of stars is supposed to be ...
... – what type of star it is, which give us… – its absolute brightness (among other things) • For example, the stars that are close enough to have their distance measured with parallax will have their spectrum analyzed. • From this, we can determine how bright a certain class of stars is supposed to be ...
STAR FORMATION (Ch. 19)
... objects to be formed in our Galaxy. Note: Abundances of all elements heavier than carbon are very small compared to the sun and most other stars (because they formed when the ...
... objects to be formed in our Galaxy. Note: Abundances of all elements heavier than carbon are very small compared to the sun and most other stars (because they formed when the ...
Study Guide: Use your notes and handouts to answer the following
... White Dwarf – Gravity squeezes all the matter of the star into a smaller space, making it more dense; eventually burns out 60. In a large star, what happens after the red giant stage? Supernova – exploding star ...
... White Dwarf – Gravity squeezes all the matter of the star into a smaller space, making it more dense; eventually burns out 60. In a large star, what happens after the red giant stage? Supernova – exploding star ...
Lecture Note
... excess of about 107 K • In the Sun, hydrogen fusion occurs in the dense, hot core ...
... excess of about 107 K • In the Sun, hydrogen fusion occurs in the dense, hot core ...
The Observer Newsletter - the TriState Astronomers
... photographing the eclipse and what you could expect to see. Fortunately, I had the presentation that George Michael created for the 2006 Eclipse in Adeta, Togo with me, and I was able to share the pictures of the 2006 total eclipse. One of the most interesting presentations was on the detection of g ...
... photographing the eclipse and what you could expect to see. Fortunately, I had the presentation that George Michael created for the 2006 Eclipse in Adeta, Togo with me, and I was able to share the pictures of the 2006 total eclipse. One of the most interesting presentations was on the detection of g ...
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.