Stellar Evolution Chapter 12
... recent maximum can be used to predict the time of a future maximum. Suppose that you calculate the time of future maximum brightness and then make measurements to observe this maximum. After the correction for Earth's orbital position has been made, you find that the maximum occurred a few minutes l ...
... recent maximum can be used to predict the time of a future maximum. Suppose that you calculate the time of future maximum brightness and then make measurements to observe this maximum. After the correction for Earth's orbital position has been made, you find that the maximum occurred a few minutes l ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
... There is a gradual increase in the helium abundance during the main-sequence phase. The increase in molecular weight results in that the core is contracting and heating up in order to provide a sufficient pressure to balance the gravity. As a consequence of this the surface layers are gradually expa ...
... There is a gradual increase in the helium abundance during the main-sequence phase. The increase in molecular weight results in that the core is contracting and heating up in order to provide a sufficient pressure to balance the gravity. As a consequence of this the surface layers are gradually expa ...
Stellar Parallax
... We do this with the following arbitarary definition:M = m when the star is viewed from a distance d = 10 pc. Then M = m -5 log10d + 5 We now have a link between M,m and d where d is in parsecs. [Note: we have assumed that the inverse square law is the only reason for the dimming of the light from th ...
... We do this with the following arbitarary definition:M = m when the star is viewed from a distance d = 10 pc. Then M = m -5 log10d + 5 We now have a link between M,m and d where d is in parsecs. [Note: we have assumed that the inverse square law is the only reason for the dimming of the light from th ...
stellar remenants
... The mass of a neutron star cannot exceed about 3 solar masses. If a core remnant is more massive than that, nothing will stop its collapse, and it will become smaller and smaller and denser and denser. Eventually the gravitational force is so intense that even light cannot escape. The remnant has be ...
... The mass of a neutron star cannot exceed about 3 solar masses. If a core remnant is more massive than that, nothing will stop its collapse, and it will become smaller and smaller and denser and denser. Eventually the gravitational force is so intense that even light cannot escape. The remnant has be ...
Diffuse Ultraviolet Emission in Galaxies
... producing large amounts of UV radiation. We divided these stars into two groups, using their traditional names: “O-type” stars, with initial masses >20 Msun and lifespans < 5 Myr, and “B-type” stars of 8–20 Msun, which live 5–25 Myr. Then we went back to the ACS exposures to investigate the location ...
... producing large amounts of UV radiation. We divided these stars into two groups, using their traditional names: “O-type” stars, with initial masses >20 Msun and lifespans < 5 Myr, and “B-type” stars of 8–20 Msun, which live 5–25 Myr. Then we went back to the ACS exposures to investigate the location ...
Chapter 8: The Pennsylvanian Period in Alabama: Looking Up
... stars formed at about the same time. The cluster known as M38 (Fig. 8.7a), one of three bright open clusters in the constellation Auriga, is as old as the Minkin site. In contrast, the Pleiades (Fig. 8.7b) are only 100 million years old. They were not shining in anybody's sky 310 million years ago. ...
... stars formed at about the same time. The cluster known as M38 (Fig. 8.7a), one of three bright open clusters in the constellation Auriga, is as old as the Minkin site. In contrast, the Pleiades (Fig. 8.7b) are only 100 million years old. They were not shining in anybody's sky 310 million years ago. ...
The Pennsylvanian Period in Alabama: Looking Up Astronomy and
... main sequence lifetimes. Since the system existed 310 million years ago, it is interesting to ask where it was at that time. Although Rigel Kent's orbit is close to ours, its distance from us and its direction in the sky vary considerably over time. 310 million years ago, it was 2,900 light years a ...
... main sequence lifetimes. Since the system existed 310 million years ago, it is interesting to ask where it was at that time. Although Rigel Kent's orbit is close to ours, its distance from us and its direction in the sky vary considerably over time. 310 million years ago, it was 2,900 light years a ...
Masses are much harder than distance, luminosity, or temperature
... brightness tracks luminosity well) • All formed about the same time (i.e. all are same age) • Range of different mass stars! ...
... brightness tracks luminosity well) • All formed about the same time (i.e. all are same age) • Range of different mass stars! ...
the life cycles of stars (5) - U3A Bendigo Courses / Activities
... Why do we see stars only in the spiral arms? Because we see only the young hot O and B stars in the arms where they are born and where they die. There are stars in the gaps between the arms but they are too faint by comparison. There is a compression shock wave which circulates around the galaxy. As ...
... Why do we see stars only in the spiral arms? Because we see only the young hot O and B stars in the arms where they are born and where they die. There are stars in the gaps between the arms but they are too faint by comparison. There is a compression shock wave which circulates around the galaxy. As ...
Starry Night Lab
... 10. Set for 9 pm, 10 days in the future. Where is the constellation you found before (higher or lower)? Go to 9 pm, 20 days from now and see where the constellation is now. 11. Summarize what you've just found: (circle the right answer) A given star rises 4 minutes [earlier/later] each night. We cal ...
... 10. Set for 9 pm, 10 days in the future. Where is the constellation you found before (higher or lower)? Go to 9 pm, 20 days from now and see where the constellation is now. 11. Summarize what you've just found: (circle the right answer) A given star rises 4 minutes [earlier/later] each night. We cal ...
1. - TeacherWeb
... • We learn about stars by studying energy. – Stars produce a full range of electromagnetic radiation, from high-energy X-rays to low-energy radio waves. – Scientists use optical telescopes to study visible light and radio telescopes to study radio waves emitted from astronomical objects. – Earth’s a ...
... • We learn about stars by studying energy. – Stars produce a full range of electromagnetic radiation, from high-energy X-rays to low-energy radio waves. – Scientists use optical telescopes to study visible light and radio telescopes to study radio waves emitted from astronomical objects. – Earth’s a ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.