PG_Lecture_Dec18_2008
... Atmospheres of “active” stars and the Sun Flare stars and the Sun have hot atmospheres, usually a corona (temperature ~ 106 K) plus a chromosphere (~10,000 K) and “transition region” (~105 K). These temperatures are generally much hotter than their surface temperatures. E.g. The Sun has surface (ph ...
... Atmospheres of “active” stars and the Sun Flare stars and the Sun have hot atmospheres, usually a corona (temperature ~ 106 K) plus a chromosphere (~10,000 K) and “transition region” (~105 K). These temperatures are generally much hotter than their surface temperatures. E.g. The Sun has surface (ph ...
Mallory, Course Implementation Using Solar System Simulator, Jan
... Make a data table listing the period of revolution/orbit time and the distance to the Sun of planets, or of the moons of planets. Then determine if there is a numeric relationship between distance to orbited body, and the time for the body to orbit. Same question as above, only for this question use ...
... Make a data table listing the period of revolution/orbit time and the distance to the Sun of planets, or of the moons of planets. Then determine if there is a numeric relationship between distance to orbited body, and the time for the body to orbit. Same question as above, only for this question use ...
Lecture 2/10 The Sun Ulf Torkelsson 1 The internal structure of the
... proton-proton-chain like in all low-mass main sequence stars. The ongoing fusion has decreased the hydrogen fraction at the centre of the star to 33 % and increased the helium fraction to 65 %. A peculiarity with the abundances in the sun is that the abundance of 3 He has a peak at 0.3R . The reaso ...
... proton-proton-chain like in all low-mass main sequence stars. The ongoing fusion has decreased the hydrogen fraction at the centre of the star to 33 % and increased the helium fraction to 65 %. A peculiarity with the abundances in the sun is that the abundance of 3 He has a peak at 0.3R . The reaso ...
Slide 1
... Conversion of Mass into Energy The nucleus of the resulting helium atom is about 0.7 percent less massive than the four component protons. ...
... Conversion of Mass into Energy The nucleus of the resulting helium atom is about 0.7 percent less massive than the four component protons. ...
Our Very Own Star: The Sun - cmase
... storms called sunspots. – They look small on the Sun but are, in fact, as large as the Earth or bigger. ...
... storms called sunspots. – They look small on the Sun but are, in fact, as large as the Earth or bigger. ...
ppt
... Construct a 1M initial model with Xini, Zini, (Yini=1- Xini-Zini) and MLT, evolve it during t and match (Z/X), L and R to better than one part in 10-5 ...
... Construct a 1M initial model with Xini, Zini, (Yini=1- Xini-Zini) and MLT, evolve it during t and match (Z/X), L and R to better than one part in 10-5 ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... Astrophysicists use computers to model the conditions within the sun. In doing so, they have been able come up with ‘facts’ about our sun. (These facts are all theoretical as it is impossible to test them) These facts include: Fusion occurs within 0.25R where temperatures reach above 10 million d ...
... Astrophysicists use computers to model the conditions within the sun. In doing so, they have been able come up with ‘facts’ about our sun. (These facts are all theoretical as it is impossible to test them) These facts include: Fusion occurs within 0.25R where temperatures reach above 10 million d ...
Why the Model of a Hydrogen
... Could this be a coincidence? Hardly! If all 83 elements in the Sun’s atmosphere were equal in abundance, the probability for the chance selection of any set of seven elements would be 7! 76! /83! = 2 x 10-10. This differs little from zero. The actual probability for chance selection of these seven e ...
... Could this be a coincidence? Hardly! If all 83 elements in the Sun’s atmosphere were equal in abundance, the probability for the chance selection of any set of seven elements would be 7! 76! /83! = 2 x 10-10. This differs little from zero. The actual probability for chance selection of these seven e ...
LETG Spring, 2015
... details of our closest cosmic source of X-rays, the Sun. Since sunspots were first reported—as far back as 2000 years ago by those precocious Chinese observers—it took until the early 1900’s and Hale’s spectrohelioscope to realize they were regions of strong magnetic field. A century later, we still ...
... details of our closest cosmic source of X-rays, the Sun. Since sunspots were first reported—as far back as 2000 years ago by those precocious Chinese observers—it took until the early 1900’s and Hale’s spectrohelioscope to realize they were regions of strong magnetic field. A century later, we still ...
Section I. SpuItering of ices ASTROPHYSICAL IMPLICATIONS OF
... particles decrease in intensity at the edge of the major A ring, so that there do not appear to be significant effects by the particles on the principal rings of Saturn. However, galactic cosmic rays do strike these ring particles, producing nuclear interactions and high energy protons and electrons ...
... particles decrease in intensity at the edge of the major A ring, so that there do not appear to be significant effects by the particles on the principal rings of Saturn. However, galactic cosmic rays do strike these ring particles, producing nuclear interactions and high energy protons and electrons ...
The Sun is our local star.
... patterns of glowing light in the sky. Such displays of light are called auroras (uh-RAWR-uhz), or the northern and southern lights. Auroras often occur near the poles. ...
... patterns of glowing light in the sky. Such displays of light are called auroras (uh-RAWR-uhz), or the northern and southern lights. Auroras often occur near the poles. ...
Kepler Mission
... DiStefano arXiv: 1002.3009 predicts order 500 orbiting WDs, neutron stars, etc will be detected by Kepler, often relying on microlensing (Sahu & Gilliland, 2003, ApJ). ...
... DiStefano arXiv: 1002.3009 predicts order 500 orbiting WDs, neutron stars, etc will be detected by Kepler, often relying on microlensing (Sahu & Gilliland, 2003, ApJ). ...
Document
... Meteorites can provide accurate information on elemental abundances in the presolar nebula. More precise than solar spectra if data in some cases. Principal source for isotopic information. But some gases escape and cannot be determined this way (for example hydrogen, or noble gases) Not all meteori ...
... Meteorites can provide accurate information on elemental abundances in the presolar nebula. More precise than solar spectra if data in some cases. Principal source for isotopic information. But some gases escape and cannot be determined this way (for example hydrogen, or noble gases) Not all meteori ...
Astronomical distances and space travel The purpose of this lab is to
... Part 1: Sattgast Hall as a scale model of the Solar System Measure the distance for the length of the hall. In order to develop an accurate scale model we will represent this length as the size of the solar system. a. Length of hall = _____________ m = Size of solar system on this scale = 40 AU. b. ...
... Part 1: Sattgast Hall as a scale model of the Solar System Measure the distance for the length of the hall. In order to develop an accurate scale model we will represent this length as the size of the solar system. a. Length of hall = _____________ m = Size of solar system on this scale = 40 AU. b. ...
From eclipse drawings to the coronagraph and spectroscopy
... the Sun is a huge plasma laboratory dynamics of a magnetized plasma how do stars and galaxies produce magnetic fields? basic physical questions: e.g. the (solved) neutrino problem ...
... the Sun is a huge plasma laboratory dynamics of a magnetized plasma how do stars and galaxies produce magnetic fields? basic physical questions: e.g. the (solved) neutrino problem ...
Test #1 Study Questions
... 3. What is the current definition of a planet? A dwarf planet? 4. Why aren’t our bones made of strontium? 5. How are minerals defined? 6. What is the R process and the S process? What are the differences? 7. What are the critical products of supernovas for solar system formation? 8. Are cosmic abund ...
... 3. What is the current definition of a planet? A dwarf planet? 4. Why aren’t our bones made of strontium? 5. How are minerals defined? 6. What is the R process and the S process? What are the differences? 7. What are the critical products of supernovas for solar system formation? 8. Are cosmic abund ...
Other Solar System Bodies
... (Figure 8.5 from K&R, reproduced overleaf). The solar wind and IMF are frozen out of the cavity occupied by the ionospheric plasma. Thus there is a bow shock upstream of Venus that acts to slow and deflect the solar wind and a magnetosheath between the topside of the ionosphere and bow shock, where ...
... (Figure 8.5 from K&R, reproduced overleaf). The solar wind and IMF are frozen out of the cavity occupied by the ionospheric plasma. Thus there is a bow shock upstream of Venus that acts to slow and deflect the solar wind and a magnetosheath between the topside of the ionosphere and bow shock, where ...
Astronomy Learning Guide Unit 04, the Sun
... solar activity. SCI.ASTR.11.4.10 Compare and contrast the origin and nature of solar granules, faculae, plages, flares, and prominences. SCI.ASTR.11.4.11 Describe the origin and nature of the solar wind. SCI.ASTR.11.4.12 Outline the goal and results of the solar neutrino ...
... solar activity. SCI.ASTR.11.4.10 Compare and contrast the origin and nature of solar granules, faculae, plages, flares, and prominences. SCI.ASTR.11.4.11 Describe the origin and nature of the solar wind. SCI.ASTR.11.4.12 Outline the goal and results of the solar neutrino ...
Pocket Solar System
... Reflection: How many more planets do we need to place? Step 7: Fold the Sun up to meet the line for Mars. Leave it folded and fold that section in half. Unfold the tape and you should have three creases. Mark the remaining planets (in proper order) at each of the creases. Pluto ...
... Reflection: How many more planets do we need to place? Step 7: Fold the Sun up to meet the line for Mars. Leave it folded and fold that section in half. Unfold the tape and you should have three creases. Mark the remaining planets (in proper order) at each of the creases. Pluto ...
solar photosphere and chromosphere
... layers above photosphere, very inhomogeneous, very dynamic a) Quiet chromosphere • spicules (Beckers 1972 [2], Wilhelm 2000 [24]): v ≈ 30 km s−1 into corona 100 times more mass than taken away by solar wind • chromospheric network: diameter ≈ 30 000 km, life time ≈ 24 h consists of boundaries, brigh ...
... layers above photosphere, very inhomogeneous, very dynamic a) Quiet chromosphere • spicules (Beckers 1972 [2], Wilhelm 2000 [24]): v ≈ 30 km s−1 into corona 100 times more mass than taken away by solar wind • chromospheric network: diameter ≈ 30 000 km, life time ≈ 24 h consists of boundaries, brigh ...
Nuclear reactions in the Sun
... • Assume this is given by the eq. of classical, perfect gases for flully ionized Hydrogen; P=nKT = (ne+np)kT =2(r/mp) kT • This can be used to derive the typical scale of T kT ≈ mp (P/r) keV ≈ 10 7 0K • This is much larger than the temperature of the photosphere, ≈ 6000 0K • The calculate profile of ...
... • Assume this is given by the eq. of classical, perfect gases for flully ionized Hydrogen; P=nKT = (ne+np)kT =2(r/mp) kT • This can be used to derive the typical scale of T kT ≈ mp (P/r) keV ≈ 10 7 0K • This is much larger than the temperature of the photosphere, ≈ 6000 0K • The calculate profile of ...
6. Solar wind acceleration
... Solar wind acceleration o The acceleration of the solar wind is considered with emphasis on the fast solar wind that is known to originate on open field lines in coronal holes, and in the smaller-scale coronal funnels. o Acceleration processes leading to slow solar wind and to transient flows driven ...
... Solar wind acceleration o The acceleration of the solar wind is considered with emphasis on the fast solar wind that is known to originate on open field lines in coronal holes, and in the smaller-scale coronal funnels. o Acceleration processes leading to slow solar wind and to transient flows driven ...
Solar phenomena
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots.These phenomena are generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations.The sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather. A major weather component is the solar wind, a stream of plasma released from the Sun's upper atmosphere. It is responsible for the aurora, natural light displays in the sky in the Arctic and Antarctic. Space weather disturbances can cause solar storms on Earth, disrupting communications, as well as geomagnetic storms in Earth's magnetosphere and sudden ionospheric disturbances in the ionosphere. Variations in solar intensity also affect Earth's climate. These variations can explain events such as ice ages and the Great Oxygenation Event, while the Sun's future expansion into a red giant will likely end life on Earth.Solar activity and related events have been recorded since the 8th century BCE. Babylonians inscribed and possibly predicted solar eclipses, while the earliest extant report of sunspots dates back to the Chinese Book of Changes, c. 800 BCE. The first extant description of the solar corona was in 968, while the earliest sunspot drawing was in 1128 and a solar prominence was described in 1185 in the Russian Chronicle of Novgorod. The invention of the telescope allowed major advances in understanding, allowing the first detailed observations in the 1600s. Solar spectroscopy began in the 1800s, from which properties of the solar atmosphere could be determined, while the creation of daguerreotypy led to the first solar photographs on 2 April 1845. Photography assisted in the study of solar prominences, granulation and spectroscopy. Early in the 20th century, interest in astrophysics surged in America. A number of new observatories were built with solar telescopes around the world. The 1931 invention of the coronagraph allowed the corona to be studied in full daylight.