Sun Physics
... Solar plasma is heated to tens of millions of degrees, and electrons, protons, and heavy nuclei are accelerated to near the speed of light. The super-heated electrons from CMEs move along the magnetic field lines faster than the solar wind can flow. Each CME releases up to 100 billion kg (220 billio ...
... Solar plasma is heated to tens of millions of degrees, and electrons, protons, and heavy nuclei are accelerated to near the speed of light. The super-heated electrons from CMEs move along the magnetic field lines faster than the solar wind can flow. Each CME releases up to 100 billion kg (220 billio ...
Homework #1: Due in class Thursday February 2nd
... Sunspots are dark patches on the Solar photosphere that mark regions where the magnetic field is strong. They are dark because the sunspot is cooler than the rest of the photosphere. Cool gases emit less thermal radiation than hot gases. Images of the Sun taken in visible light and X-rays appear ver ...
... Sunspots are dark patches on the Solar photosphere that mark regions where the magnetic field is strong. They are dark because the sunspot is cooler than the rest of the photosphere. Cool gases emit less thermal radiation than hot gases. Images of the Sun taken in visible light and X-rays appear ver ...
The Sun: Our Star (Chapter 14) The source of the Sun`s energy has
... is kept constant by a “thermostat” that increases the rate if it decreases too much and decreases the rate if it increases too much. Energy generated by nuclear fusion keeps the pressure within the Sun high. This supports the weight of the Sun. It takes 100,000 years for energy to move out through t ...
... is kept constant by a “thermostat” that increases the rate if it decreases too much and decreases the rate if it increases too much. Energy generated by nuclear fusion keeps the pressure within the Sun high. This supports the weight of the Sun. It takes 100,000 years for energy to move out through t ...
The Sun*s
... High-speed charged particles (mostly electrons and protons) constantly blowing off the Sun. May be viewed as an extension of the outer atmosphere of the Sun (the corona) into interplanetary space. Computer image ...
... High-speed charged particles (mostly electrons and protons) constantly blowing off the Sun. May be viewed as an extension of the outer atmosphere of the Sun (the corona) into interplanetary space. Computer image ...
chapter7
... The solar interior is opaque (i.e. it absorbs light) out to the photosphere. Only way to investigate ...
... The solar interior is opaque (i.e. it absorbs light) out to the photosphere. Only way to investigate ...
Scales of the Universe
... you looked at the Sun’s photosphere now? • The photosphere: the region where the black body radiation that we see is made • Thin gas: 3,400 times thinner than air • It is the transition region from a black-body emitting plasma to a transparent gas • Its upper layer produces the absorption spectrum • ...
... you looked at the Sun’s photosphere now? • The photosphere: the region where the black body radiation that we see is made • Thin gas: 3,400 times thinner than air • It is the transition region from a black-body emitting plasma to a transparent gas • Its upper layer produces the absorption spectrum • ...
Document
... • The Sun’s energy comes from nuclear fusion – the merging of hydrogen nuclei into helium. • Each fusion reaction releases only a little bit of energy, but it happens a lot. • A helium nucleus has less mass than the four protons (hydrogen nuclei) that fuse to create it. • This difference in mass is ...
... • The Sun’s energy comes from nuclear fusion – the merging of hydrogen nuclei into helium. • Each fusion reaction releases only a little bit of energy, but it happens a lot. • A helium nucleus has less mass than the four protons (hydrogen nuclei) that fuse to create it. • This difference in mass is ...
Exam 3 Solution Set - Indiana University Astronomy
... Since E=mc2, the energy produced is 6.5 x 1029 x 9 x 1020 ergs = 5.9 x 1050 ergs. The main sequence lifetime of the Sun is about 1010 years, and the luminosity of the sun is 4 x 1033 ergs s-1. During its main sequence lifetime, the sun produces 3 x 107 s year-1 x 1010 years x 4 x 1033 ergs s-1 = 1.2 ...
... Since E=mc2, the energy produced is 6.5 x 1029 x 9 x 1020 ergs = 5.9 x 1050 ergs. The main sequence lifetime of the Sun is about 1010 years, and the luminosity of the sun is 4 x 1033 ergs s-1. During its main sequence lifetime, the sun produces 3 x 107 s year-1 x 1010 years x 4 x 1033 ergs s-1 = 1.2 ...
The Sun - www .alexandria .k12 .mn .us
... • Prominences (aka coronal loops) are large, bright loop-shaped features on the photosphere that extend out into the corona • A prominence takes ~1 day to form and may persist for several months. • A typical prominence extends over many 1000s of kms; the largest recorded was over 800000 kms long ...
... • Prominences (aka coronal loops) are large, bright loop-shaped features on the photosphere that extend out into the corona • A prominence takes ~1 day to form and may persist for several months. • A typical prominence extends over many 1000s of kms; the largest recorded was over 800000 kms long ...
12-Sun
... A sudden brightening, above large spot group, between regions of opposite polarity Outburst of charged particles (cosmic rays), increase in high energy radiation ...
... A sudden brightening, above large spot group, between regions of opposite polarity Outburst of charged particles (cosmic rays), increase in high energy radiation ...
Notes: Sun
... 1. Does the Sun have a solid surface? 2. Since the Sun is so bright, how is it possible to see its dim outer atmosphere? 3. Where does the solar wind come from? 4. What are sunspots? Why do they appear dark? 5. What is the connection between sunspots and the Sun’s magnetic field? 6. What causes erup ...
... 1. Does the Sun have a solid surface? 2. Since the Sun is so bright, how is it possible to see its dim outer atmosphere? 3. Where does the solar wind come from? 4. What are sunspots? Why do they appear dark? 5. What is the connection between sunspots and the Sun’s magnetic field? 6. What causes erup ...
The Sun as a Star
... Sunspots, prominences, flares all associated with magnetic fields All increase and reach maximum with 11 yr solar activity cycle ...
... Sunspots, prominences, flares all associated with magnetic fields All increase and reach maximum with 11 yr solar activity cycle ...
Our Sun is a Star:
... If you built a super fast space shuttle that could fly from the sun to the earth in one day, how long would you think it should take to fly from the earth to Pluto based on the information in this map? (I’m asking for an estimate so there is no right or wrong answer) ...
... If you built a super fast space shuttle that could fly from the sun to the earth in one day, how long would you think it should take to fly from the earth to Pluto based on the information in this map? (I’m asking for an estimate so there is no right or wrong answer) ...
ASTRO REVIEW 14
... _____ 9. What theory states that the universe began in a violent explosion? a. Doppler effect ...
... _____ 9. What theory states that the universe began in a violent explosion? a. Doppler effect ...
Magnetic Fields of Sun PowerPoint
... active regions are places where the magnetic field is especially strong and often produces sunspots. Disruptions in magnetic fields near active regions can cause explosions on the sun such as solar flares and Coronal Mass ...
... active regions are places where the magnetic field is especially strong and often produces sunspots. Disruptions in magnetic fields near active regions can cause explosions on the sun such as solar flares and Coronal Mass ...
Document
... • Hot, low density, gas emits the radiation we see as the Corona: 1,000,000 K • Solar Wind: Like steam above our boiling pot of water, the gas ‘evaporates’. • Carries away a million tons of Sun’s mass each second! • Only 0.1% of total Sun’s mass in last 4.6 billion years. ...
... • Hot, low density, gas emits the radiation we see as the Corona: 1,000,000 K • Solar Wind: Like steam above our boiling pot of water, the gas ‘evaporates’. • Carries away a million tons of Sun’s mass each second! • Only 0.1% of total Sun’s mass in last 4.6 billion years. ...
Document
... Photosphere -- light sphere The surface in “visible” light T ~ 6500 - 4000 K Depth 100’s kms ...
... Photosphere -- light sphere The surface in “visible” light T ~ 6500 - 4000 K Depth 100’s kms ...
Steve Tomczyk & Scott McIntosh - National Center for Atmospheric
... consisting of seven engineers and three interns collaborates with HAO scientists to develop state-ofthe-art instruments for the observation of the Sun and the Earth’s upper atmosphere. Scott received his bachelors degree in Astronomy from Villanova University in 1979 and went on to graduate study at ...
... consisting of seven engineers and three interns collaborates with HAO scientists to develop state-ofthe-art instruments for the observation of the Sun and the Earth’s upper atmosphere. Scott received his bachelors degree in Astronomy from Villanova University in 1979 and went on to graduate study at ...
The Sun - Moodle
... and the corona is the chromosphere (sphere of ________________) Corona—atmosphere outermost region extends out several million kilometers and merges into a hurricane of high-speed protons and electrons called the ______________ _ ...
... and the corona is the chromosphere (sphere of ________________) Corona—atmosphere outermost region extends out several million kilometers and merges into a hurricane of high-speed protons and electrons called the ______________ _ ...
The Corona
... This produced a really strange emission spectrum. This layer emits most of its radiation at very short UV an X-ray wavelengths. Much of this radiation hits Earth’s atmosphere and is absorbed by atoms and molecules. So, scientists use instruments in space to study the Corona. The Corona is visible du ...
... This produced a really strange emission spectrum. This layer emits most of its radiation at very short UV an X-ray wavelengths. Much of this radiation hits Earth’s atmosphere and is absorbed by atoms and molecules. So, scientists use instruments in space to study the Corona. The Corona is visible du ...
Corona
A corona (Latin, 'crown') is an aura of plasma that surrounds the sun and other celestial bodies. The Sun's corona extends millions of kilometres into space and is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The word ""corona"" is a Latin word meaning ""crown"", from the Ancient Greek κορώνη (korōnē, “garland, wreath”).The high temperature of the Sun's corona gives it unusual spectral features, which led some in the 19th century to suggest that it contained a previously unknown element, ""coronium"". Instead, these spectral features have since been explained by highly ionized iron (Fe-XIV). Bengt Edlén, following the work of Grotrian (1939), first identified the coronal lines in 1940 (observed since 1869) as transitions from low-lying metastable levels of the ground configuration of highly ionised metals (the green Fe-XIV line at 5303 Å, but also the red line Fe-X at 6374 Å). These high stages of ionisation indicate a plasma temperature in excess of 1,000,000 kelvin, much hotter than the surface of the sun.Light from the corona comes from three primary sources, which are called by different names although all of them share the same volume of space. The K-corona (K for kontinuierlich, ""continuous"" in German) is created by sunlight scattering off free electrons; Doppler broadening of the reflected photospheric absorption lines completely obscures them, giving the spectral appearance of a continuum with no absorption lines. The F-corona (F for Fraunhofer) is created by sunlight bouncing off dust particles, and is observable because its light contains the Fraunhofer absorption lines that are seen in raw sunlight; the F-corona extends to very high elongation angles from the Sun, where it is called the zodiacal light. The E-corona (E for emission) is due to spectral emission lines produced by ions that are present in the coronal plasma; it may be observed in broad or forbidden or hot spectral emission lines and is the main source of information about the corona's composition.