Study Questions for Test 2
... What are observational advantages of locating a telescope on a mountain top? Which forms of electromagnetic radiation reach Earth’s surface and which forms are blocked by ozone and water vapor in Earth’s atmosphere? What are the three “powers” an optical telescope? Rank their importance. What is ada ...
... What are observational advantages of locating a telescope on a mountain top? Which forms of electromagnetic radiation reach Earth’s surface and which forms are blocked by ozone and water vapor in Earth’s atmosphere? What are the three “powers” an optical telescope? Rank their importance. What is ada ...
sources of hard and soft x-ray emission in solar flares: mhd simulation
... Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia, podgorny@inasan.ru Primordial energy release during the solar flare on height 15000–30000 km is explained by appearance of the current sheet in the magnetic field of the solar corona above the active region. The energy ~1032 erg, w ...
... Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia, podgorny@inasan.ru Primordial energy release during the solar flare on height 15000–30000 km is explained by appearance of the current sheet in the magnetic field of the solar corona above the active region. The energy ~1032 erg, w ...
RAS_waves - University of Glasgow
... 1) Pre-flare energy storage => twisted field, so energy release => untwisting – i.e. an Alfvenic pulse. Consequences? 2) Earth’s magnetosphere provides an example of efficient particle acceleration by Alfven waves, generated in substorms. 1) Since the (1970s) it is clear that the corona contains ins ...
... 1) Pre-flare energy storage => twisted field, so energy release => untwisting – i.e. an Alfvenic pulse. Consequences? 2) Earth’s magnetosphere provides an example of efficient particle acceleration by Alfven waves, generated in substorms. 1) Since the (1970s) it is clear that the corona contains ins ...
23sun4s
... The solar interior is the source of solar energy which is transported to the surface Nuclear fusion and magnetic fields play key roles in the energetics and structure of the Sun ...
... The solar interior is the source of solar energy which is transported to the surface Nuclear fusion and magnetic fields play key roles in the energetics and structure of the Sun ...
Ch 29 Sun and Solar Activity
... Changes to Sun’s features over periods of time…caused by the Sun’s magnetic field ...
... Changes to Sun’s features over periods of time…caused by the Sun’s magnetic field ...
9.1: THE SUN IN BULK PHYS 1401: Descriptive Astronomy Notes
... origin in lower atmosphere, can reach 100,000,000K (hotter than solar core) ✦ Coronal Mass Ejection: Bubble of ionized/magnetized gas detaches from corona; number of CMEs increases with sunspot activity; potential to disrupt e·m fields on Earth ...
... origin in lower atmosphere, can reach 100,000,000K (hotter than solar core) ✦ Coronal Mass Ejection: Bubble of ionized/magnetized gas detaches from corona; number of CMEs increases with sunspot activity; potential to disrupt e·m fields on Earth ...
Lecture 2/10 The Sun Ulf Torkelsson 1 The internal structure of the
... 1000 K lower than the rest of the photosphere. These sunspots have strong magnetic fields on the order of 0.1 T. The reason that the sun spots are cooler appears to be that the magnetic field is suppressing the convection beneath the sun spot, so that it receives less heat than other parts of the so ...
... 1000 K lower than the rest of the photosphere. These sunspots have strong magnetic fields on the order of 0.1 T. The reason that the sun spots are cooler appears to be that the magnetic field is suppressing the convection beneath the sun spot, so that it receives less heat than other parts of the so ...
The Sun
... because of the twisted magnetic fields disrupting convection, finds its way out in surrounding areas. In fact, the magnetic field energy created actually makes the sun a bit BRIGHTER with higher solar activity. • These surrounding areas are called Plages • Here’s a black/white picture up close… ...
... because of the twisted magnetic fields disrupting convection, finds its way out in surrounding areas. In fact, the magnetic field energy created actually makes the sun a bit BRIGHTER with higher solar activity. • These surrounding areas are called Plages • Here’s a black/white picture up close… ...
Solar Wind/Outer Magnetosphere
... • Coronal Mass Ejections (CMEs) • Large eruptions of coronal plasma from the Sun • Eruption occurs over several hours • Magnetic field is often complex (this is important for interactions with Earth’s magnetosphere) • Shock front travels ahead of CME (also important for interactions with Earth’s mag ...
... • Coronal Mass Ejections (CMEs) • Large eruptions of coronal plasma from the Sun • Eruption occurs over several hours • Magnetic field is often complex (this is important for interactions with Earth’s magnetosphere) • Shock front travels ahead of CME (also important for interactions with Earth’s mag ...
Chapter 5 Essay Questions
... 3 What is the definition of density? Approximately, what is the average density of the sun? 4 The corona is much hotter than the photosphere, yet we have to wait for a total solar eclipse to see the corona. Why is that? 5 Suppose you have a cool gas cloud of atoms, and you send visible light of all ...
... 3 What is the definition of density? Approximately, what is the average density of the sun? 4 The corona is much hotter than the photosphere, yet we have to wait for a total solar eclipse to see the corona. Why is that? 5 Suppose you have a cool gas cloud of atoms, and you send visible light of all ...
Sunspots Magnetic Field
... photons of natural visible light, mostly unpolarized. It is sprinkled with small dark, relatively cool areas called sunspots, which are regions of strong magnetic field on the photosphere. Sunspot temperature is 4000 K compared to 6000 K elsewhere in the photosphere. Sunspot magnetic field is about ...
... photons of natural visible light, mostly unpolarized. It is sprinkled with small dark, relatively cool areas called sunspots, which are regions of strong magnetic field on the photosphere. Sunspot temperature is 4000 K compared to 6000 K elsewhere in the photosphere. Sunspot magnetic field is about ...
The Sun and Space Weather
... dammage effects; deep dielecrtic charging (responsible for anomalies and losses); surface charging anomalies. ...
... dammage effects; deep dielecrtic charging (responsible for anomalies and losses); surface charging anomalies. ...
the Sun - University of Redlands
... – Closer to surface, the temperature is cooler. – Atoms are no longer ionized. – Electrons around nuclei can absorb light from below. ...
... – Closer to surface, the temperature is cooler. – Atoms are no longer ionized. – Electrons around nuclei can absorb light from below. ...
Coronal Mass Ejection
... • Coronal mass ejections (CMJ) can occur at any point in the cycle. Flares are also unpredictable. • Solar flares and CMJ’s produce showers of charged particles (electrons and protons). • Can disrupt electrical grids, radio and TV transmissions. ...
... • Coronal mass ejections (CMJ) can occur at any point in the cycle. Flares are also unpredictable. • Solar flares and CMJ’s produce showers of charged particles (electrons and protons). • Can disrupt electrical grids, radio and TV transmissions. ...
Lesson 6 The Sun and its power source
... of the chromosphere Very low density – only visible during an eclipse Extremely hot! (1 to 2 million K) ...
... of the chromosphere Very low density – only visible during an eclipse Extremely hot! (1 to 2 million K) ...
Week 3 - Emerson Valley School
... planets across our solar system. These spherical bodies march across the sky in a predictable way: the length of their days and years remaining reliably constant. Although scientists have learned a great deal about the solar system, there are still further questions to answer and many mysteries to e ...
... planets across our solar system. These spherical bodies march across the sky in a predictable way: the length of their days and years remaining reliably constant. Although scientists have learned a great deal about the solar system, there are still further questions to answer and many mysteries to e ...
GLOSSARY
... Solar Corona :【太陽コロナ】 Hot and extended atmosphere surrounding the Sun whose temperature is more than one million K. We can see the solar corona at the visible light when the strong radiation of the solar disk is blocked in a total solar eclipse. We can observe the solar corona in X-rays and UVs from ...
... Solar Corona :【太陽コロナ】 Hot and extended atmosphere surrounding the Sun whose temperature is more than one million K. We can see the solar corona at the visible light when the strong radiation of the solar disk is blocked in a total solar eclipse. We can observe the solar corona in X-rays and UVs from ...
Quiz #5 – The Sun
... Compared to the Earth’s diameter, the sun’s diameter is about 110 times greater. ...
... Compared to the Earth’s diameter, the sun’s diameter is about 110 times greater. ...
The Sun
... Finally, the eruption becomes a prominence as the magnetic energy from the PHOTOSPHERE reaches the CORONA hurling the MAGNETIC ...
... Finally, the eruption becomes a prominence as the magnetic energy from the PHOTOSPHERE reaches the CORONA hurling the MAGNETIC ...
The Sun
... •On the sun this is the area where the energy from the core is filtered and circulates. •It is the upper 15% of the sun’s interior, and is ...
... •On the sun this is the area where the energy from the core is filtered and circulates. •It is the upper 15% of the sun’s interior, and is ...
Document
... • In a matter of just a few minutes they heat material to many millions of degrees and release as much energy as a billion megatons of TNT. ...
... • In a matter of just a few minutes they heat material to many millions of degrees and release as much energy as a billion megatons of TNT. ...
Chapter 20 Notes: Solar System The Solar System Sun’s Interior
... Corona Corona means crown Looks like a white halo Only seen during a total solar eclipse extends millions of kilometers into space as solar wind ...
... Corona Corona means crown Looks like a white halo Only seen during a total solar eclipse extends millions of kilometers into space as solar wind ...
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.