First Light Sources at the End of the Dark Ages: Direct
... emission-line characteristics. The longevity of the emission lines makes their detection and study conventional observations that require a baseline of 2-10 years. These are not target of opportunity observations. Undertaking searches for SNe IIn out to high redshift will reveal the evolving fractio ...
... emission-line characteristics. The longevity of the emission lines makes their detection and study conventional observations that require a baseline of 2-10 years. These are not target of opportunity observations. Undertaking searches for SNe IIn out to high redshift will reveal the evolving fractio ...
2.1 Introduction
... youngest stellar clusters known, with an age of only 1 million years. It is associated with the Carina nebula at a distance of 3.2 kpc. It is immediately obvious from these images that: (a) stars have a range of colours, and (b) some stars are intrinsically brighter than others. More generally, we c ...
... youngest stellar clusters known, with an age of only 1 million years. It is associated with the Carina nebula at a distance of 3.2 kpc. It is immediately obvious from these images that: (a) stars have a range of colours, and (b) some stars are intrinsically brighter than others. More generally, we c ...
Chapter 29
... The nebulae collapses upon itself and rotates. As it continues to contract it gains pressure and temperature until fusion begins ...
... The nebulae collapses upon itself and rotates. As it continues to contract it gains pressure and temperature until fusion begins ...
Lecture16
... We recently added two new spectral types to this list. The “L”s and “T”s. Their temperatures range from 2500 K down to 700 K. These types generally contain the very lowest mass stars and “brown dwarfs”. Brown dwarfs have so little mass, they cannot even start nuclear fusion. ...
... We recently added two new spectral types to this list. The “L”s and “T”s. Their temperatures range from 2500 K down to 700 K. These types generally contain the very lowest mass stars and “brown dwarfs”. Brown dwarfs have so little mass, they cannot even start nuclear fusion. ...
Theory of the Infinite Universe
... structure. But this process is not infinite. Eventually the structure will reach a point where the gravitational forces break up the building blocks of elementary particles (neutrons, protons, electrons) ...
... structure. But this process is not infinite. Eventually the structure will reach a point where the gravitational forces break up the building blocks of elementary particles (neutrons, protons, electrons) ...
Document
... or RJ ~ GmHM/3kT Cloud fragments & collapses if M>MJ, R>RJ Free-fall time = (3/32Go)1/2 for T~150K, n~108/cm3, ~2x10-16 g/cm3 ...
... or RJ ~ GmHM/3kT Cloud fragments & collapses if M>MJ, R>RJ Free-fall time = (3/32Go)1/2 for T~150K, n~108/cm3, ~2x10-16 g/cm3 ...
Chapter 15
... the hydrogen fuel in its core to make helium. The helium is basically just sitting there, so it's not producing any energy. Instead, the core is shrinking and getting hotter. Before long, it'll get hot enough to ignite the helium, which will begin fusing together to make heavier elements. When that ...
... the hydrogen fuel in its core to make helium. The helium is basically just sitting there, so it's not producing any energy. Instead, the core is shrinking and getting hotter. Before long, it'll get hot enough to ignite the helium, which will begin fusing together to make heavier elements. When that ...
Announcements
... random orbits passing close to center Later, rotation made any remaining gas flatten into disk. Stars forming after this have orbits in disk. ...
... random orbits passing close to center Later, rotation made any remaining gas flatten into disk. Stars forming after this have orbits in disk. ...
Components of the Universe Test Review
... 3. the sun is still the center of the universe 4. all objects in the universe are the same distance apart ...
... 3. the sun is still the center of the universe 4. all objects in the universe are the same distance apart ...
WORD - hrsbstaff.ednet.ns.ca
... (b) The region on the H-R diagram where, once they are formed. new stars rest for most of their lives. (c) The sequence of events a star follows from its formation to supernova. (d) The region on the H-R diagram where protostars first appear. 50. Define hydrogen burning. (a) The formation of a hydro ...
... (b) The region on the H-R diagram where, once they are formed. new stars rest for most of their lives. (c) The sequence of events a star follows from its formation to supernova. (d) The region on the H-R diagram where protostars first appear. 50. Define hydrogen burning. (a) The formation of a hydro ...
Powerpoint Presentation (large file)
... star when core helium fusion begins – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
... star when core helium fusion begins – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
1 WHY DO THE STARS IN ORION LOOK SO DIFFERENT FROM
... Table 1 is Rigel, with an mv of 0.12, which happens to also be the brightest star in the Orion constellation. The apparent magnitude is as we observe the star from earth. It is not reflective of a stars true physical character, such as its size or luminosity. More on these later. The second stars in ...
... Table 1 is Rigel, with an mv of 0.12, which happens to also be the brightest star in the Orion constellation. The apparent magnitude is as we observe the star from earth. It is not reflective of a stars true physical character, such as its size or luminosity. More on these later. The second stars in ...
Astro 210 Lecture 4 Sept. 4, 2013 Announcements: • PS 1 available
... Q: how do we know they are giant? a rare few: hot but luminous: “supergiants” not rare but dim and hard to find: very hot but very low-L objects: “white dwarfs” Q: how do we know they are teeny? ...
... Q: how do we know they are giant? a rare few: hot but luminous: “supergiants” not rare but dim and hard to find: very hot but very low-L objects: “white dwarfs” Q: how do we know they are teeny? ...
English Summary
... Enrichment of the interstellar medium We have seen that the gas from which the stars are formed consist mostly of hydrogen. Through the ejection of their envelope, Planetary Nebulae return gas to the interstellar medium from which future generations of stars will be formed. This gas still contains m ...
... Enrichment of the interstellar medium We have seen that the gas from which the stars are formed consist mostly of hydrogen. Through the ejection of their envelope, Planetary Nebulae return gas to the interstellar medium from which future generations of stars will be formed. This gas still contains m ...
Devil physics The baddest class on campus IB Physics
... forced into the same quantum state Pauli exclusion principle says they will acquire large kinetic energy which allows the star to resist gravitational pressure to collapse ...
... forced into the same quantum state Pauli exclusion principle says they will acquire large kinetic energy which allows the star to resist gravitational pressure to collapse ...
Model of Stars—6 Oct Test 1: Average 17 (75%) •
... People emit light in the “thermal infrared” part of the spectrum. Your eyes cannot see infrared radiation. 8000< <12000nm You can see visible light • Blue 440nm • Green 550nm • Red 620nm ...
... People emit light in the “thermal infrared” part of the spectrum. Your eyes cannot see infrared radiation. 8000< <12000nm You can see visible light • Blue 440nm • Green 550nm • Red 620nm ...
Astronomy Final Study Guide – Name: **This will be the biggest test
... **This will be the biggest test we have taken this year. I recommend using this study guide wisely to analyze what you already know well. Ask your friends questions. Quiz each other. Ask me questions. There is no point in copying each other because this is not a homework assignment, but it will help ...
... **This will be the biggest test we have taken this year. I recommend using this study guide wisely to analyze what you already know well. Ask your friends questions. Quiz each other. Ask me questions. There is no point in copying each other because this is not a homework assignment, but it will help ...
2 - BYU Physics and Astronomy
... A-6. The track of a star which rises directly in the east is shown with respect to an observer's horizon. The observer's location is (a) near but not at the north pole, (b) at an intermediate northern latitude, (c) near but slightly north of the equator, (d) on the equator, (e) near but slightly sou ...
... A-6. The track of a star which rises directly in the east is shown with respect to an observer's horizon. The observer's location is (a) near but not at the north pole, (b) at an intermediate northern latitude, (c) near but slightly north of the equator, (d) on the equator, (e) near but slightly sou ...
chap17_f03_phints
... A star is determined to have a surface temperature twice that of the Sun, and a luminosity 64X greater. What is this star’s radius, expressed in solar units ? HINT: Problem 4 is an application of the radius – luminosity – temperature relation for stars. Given two of these values, the third is found ...
... A star is determined to have a surface temperature twice that of the Sun, and a luminosity 64X greater. What is this star’s radius, expressed in solar units ? HINT: Problem 4 is an application of the radius – luminosity – temperature relation for stars. Given two of these values, the third is found ...
Passport to the Universe Educator`s Guide Text
... the Earth and the other planets in the larger scheme of things. From out here, the sizes of and distances between the Earth, Sun, and other planets appear relatively small. On our trip, we pass three of the eight planets—Mars, Jupiter (and its moons, Io and Europa), and Saturn. We now head out for ...
... the Earth and the other planets in the larger scheme of things. From out here, the sizes of and distances between the Earth, Sun, and other planets appear relatively small. On our trip, we pass three of the eight planets—Mars, Jupiter (and its moons, Io and Europa), and Saturn. We now head out for ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.