Planetarium Key Points
... The stars seem numberless and there are actually more than 2 billions of stars in the system we live in (Milky Way), but only 3000 stars are visible at naked eye What we see is NOT what it is actually, the response of our eye is logarithmic not linear All celestial objects seem at the same dis ...
... The stars seem numberless and there are actually more than 2 billions of stars in the system we live in (Milky Way), but only 3000 stars are visible at naked eye What we see is NOT what it is actually, the response of our eye is logarithmic not linear All celestial objects seem at the same dis ...
The Sun and other Stars
... A star’s spectral class is determined by the lines in its spectrum Hot objects are blue and cool objects are red. Class O & B stars are bluish, K & M stars are reddish. ...
... A star’s spectral class is determined by the lines in its spectrum Hot objects are blue and cool objects are red. Class O & B stars are bluish, K & M stars are reddish. ...
Spectroscopy Lecture 10
... – Found Sirius B at Northwestern’s Dearborn Observatory Procyon B found in 1895 at Lick – Was it a star that had cooled and dimmed? Spectrum of 40 Eri B observed – an A star! – It must be hot – Must have small radius to be so faint – The first “w hite dwarf” Adams found Sirius B is also an A star ...
... – Found Sirius B at Northwestern’s Dearborn Observatory Procyon B found in 1895 at Lick – Was it a star that had cooled and dimmed? Spectrum of 40 Eri B observed – an A star! – It must be hot – Must have small radius to be so faint – The first “w hite dwarf” Adams found Sirius B is also an A star ...
Powerpoint file
... Short period M dwarfs are very active and we would have seen Ca II emission from the binary stars and X-ray emission ...
... Short period M dwarfs are very active and we would have seen Ca II emission from the binary stars and X-ray emission ...
Lec8_2D
... absorption lines changes with time (redshift, then blueshift, then redshift, etc.), it’s a spectroscopic binary. If one star is much fainter than the other, you may not see its lines. The object is then a singleline spectroscopic binary. If both sets of lines are seen, then it’s called a double-line ...
... absorption lines changes with time (redshift, then blueshift, then redshift, etc.), it’s a spectroscopic binary. If one star is much fainter than the other, you may not see its lines. The object is then a singleline spectroscopic binary. If both sets of lines are seen, then it’s called a double-line ...
PHYSICS – Astrophysics Section I
... Discuss Galileo’s use of the telescope to identify features of the Moon In 1609, Galileo constructed his own powerful telescope after hearing about its ability to make objects look closer. He used it to observe many phenomenon of the Solar System, including features of the Moon. Galileo saw that the ...
... Discuss Galileo’s use of the telescope to identify features of the Moon In 1609, Galileo constructed his own powerful telescope after hearing about its ability to make objects look closer. He used it to observe many phenomenon of the Solar System, including features of the Moon. Galileo saw that the ...
White Dwarfs and Neutron Stars
... • Does a more massive white dwarf have a larger or smaller radius than a less massive one? • What is the maximum mass of a white dwarf? • What are some of the properties of neutron stars? • Why do many neutron stars spin rapidly? • In what different forms does one find neutron stars? ...
... • Does a more massive white dwarf have a larger or smaller radius than a less massive one? • What is the maximum mass of a white dwarf? • What are some of the properties of neutron stars? • Why do many neutron stars spin rapidly? • In what different forms does one find neutron stars? ...
How Old is the Universe?
... that the age of the Universe is greater than 12.07 Gyr with 95% confidence. They say the age is proportional to one over the luminosity of the RR Lyra stars which are used to determine the distances to globular clusters. Chaboyer (1997) gives a best estimate of 14.6 +/- 1.7 Gyr for the age of the gl ...
... that the age of the Universe is greater than 12.07 Gyr with 95% confidence. They say the age is proportional to one over the luminosity of the RR Lyra stars which are used to determine the distances to globular clusters. Chaboyer (1997) gives a best estimate of 14.6 +/- 1.7 Gyr for the age of the gl ...
File
... • Hydrogen and most of the helium in the universe are primordial, that is they date from the earliest times. • All other elements in the universe are a result of stellar nucleosynthesis: they were formed by nuclear fusion in the heart of stars. (also by processes occurring in supernovae) ...
... • Hydrogen and most of the helium in the universe are primordial, that is they date from the earliest times. • All other elements in the universe are a result of stellar nucleosynthesis: they were formed by nuclear fusion in the heart of stars. (also by processes occurring in supernovae) ...
13 Space Photos To Remind You The Universe Is
... nebulae (like the Helix Nebula above) are actually the remains of stars that once looked a lot like our sun. These stars spend most of their lives turning hydrogen into helium in massive runaway nuclear fusion reactions in their cores. ...
... nebulae (like the Helix Nebula above) are actually the remains of stars that once looked a lot like our sun. These stars spend most of their lives turning hydrogen into helium in massive runaway nuclear fusion reactions in their cores. ...
Star Birth
... Thought Question What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A. It would continue contracting, but its temperature would not change B. Its mass would increase C. Its internal pressure would increase ...
... Thought Question What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A. It would continue contracting, but its temperature would not change B. Its mass would increase C. Its internal pressure would increase ...
Devika kamath Institute of Astronomy, KU. Leuven, Belgium
... TO THE OBSERVATIONAL FIELDS OF THE POST-RGB STARS The number of stars we expect to see at any given time in the top 1 magnitude of the RGB is k = 2.77 x106 × birthrate tip-RGB Total number of stars observed in the top 1 magnitude of the RGB in the fields searched for post-RGB stars is 118927 (from S ...
... TO THE OBSERVATIONAL FIELDS OF THE POST-RGB STARS The number of stars we expect to see at any given time in the top 1 magnitude of the RGB is k = 2.77 x106 × birthrate tip-RGB Total number of stars observed in the top 1 magnitude of the RGB in the fields searched for post-RGB stars is 118927 (from S ...
ALUMINIUM-26 IN THE EARLY SOLAR SYSTEM : A PROBABILITY
... when massive stars are ready to explode as SNe, they are surrounded by HII regions of radius a few pc where star formation does not occur [21]. If that constraint had been taken into account by [7, 8], the probability estimate for a single SN would have been close to zero. The number of a few % is i ...
... when massive stars are ready to explode as SNe, they are surrounded by HII regions of radius a few pc where star formation does not occur [21]. If that constraint had been taken into account by [7, 8], the probability estimate for a single SN would have been close to zero. The number of a few % is i ...
BENNETT, Constraints on the Orbital Motion of OGLE-2006
... • OGLE images show that the source is offset from the bright star by 350 mas • B. Macintosh: Keck AO images resolve lens+source stars from the brighter star. • But, source+lens blend is 6 brighter than the source (from CTIO H-band light curve), so the lens star is 5 brighter than source. – H-band ...
... • OGLE images show that the source is offset from the bright star by 350 mas • B. Macintosh: Keck AO images resolve lens+source stars from the brighter star. • But, source+lens blend is 6 brighter than the source (from CTIO H-band light curve), so the lens star is 5 brighter than source. – H-band ...
Ch. 17 (RGs & WDs)
... from main-sequence one in the same spectral class • If spectrum is measured, can find luminosity; combining this with apparent brightness allows distance to be calculated ...
... from main-sequence one in the same spectral class • If spectrum is measured, can find luminosity; combining this with apparent brightness allows distance to be calculated ...
Star Formation - University of Redlands
... – Opaque to blue light, UV, X-rays – Transparent to red light, IR, radio ...
... – Opaque to blue light, UV, X-rays – Transparent to red light, IR, radio ...
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.