STARS In your textbook, read about the properties of the Sun and
... has a temperature of nearly 30,000 Kat the top. Without special filters, this layer is visible only during a ...
... has a temperature of nearly 30,000 Kat the top. Without special filters, this layer is visible only during a ...
The Sun - TutorPlus
... contains ‘spike like’ prominences, called spicules, that rise like geysers carrying magnetic fields. ...
... contains ‘spike like’ prominences, called spicules, that rise like geysers carrying magnetic fields. ...
ASTRONOMY 1001 FALL SEMESTER 2004
... momentum, interstellar clouds, gravitational contraction, accretion, planetesimals, protoplanets, collisions, solar wind 3) Sun: Structure, photosphere, chromosphere, corona, sunspots, prominences, flares, granulation, solar wind, aurorae Energy transport, convection, radiation, conduction Gravitati ...
... momentum, interstellar clouds, gravitational contraction, accretion, planetesimals, protoplanets, collisions, solar wind 3) Sun: Structure, photosphere, chromosphere, corona, sunspots, prominences, flares, granulation, solar wind, aurorae Energy transport, convection, radiation, conduction Gravitati ...
Structure of the Sun
... 2) During eclipses it glows a reddish color, this color is given off by the hydrogen 3) Temperatures range from 4,000 – 50,000 degrees C 4) In upward movements, gas regularly forms narrow jets of hot gas that shoot outward to form the chromospheres and then fade way within a few minutes. a. They can ...
... 2) During eclipses it glows a reddish color, this color is given off by the hydrogen 3) Temperatures range from 4,000 – 50,000 degrees C 4) In upward movements, gas regularly forms narrow jets of hot gas that shoot outward to form the chromospheres and then fade way within a few minutes. a. They can ...
Solar Plasmas - Coalition for Plasma Science
... particles and magnetic fields, interacts with the interplanetary environment and produces “space weather,” creating effects on earth both beautiful (auroras) and destructive (power and communication blackouts). While in many respects the sun is an average star, it is 260 thousand times closer than a ...
... particles and magnetic fields, interacts with the interplanetary environment and produces “space weather,” creating effects on earth both beautiful (auroras) and destructive (power and communication blackouts). While in many respects the sun is an average star, it is 260 thousand times closer than a ...
The Sun
... – At the photosphere, the density is so low that the gas is again transparent to light. – The hot convection cell tops radiate energy as a function of their temperature (5800 K). ...
... – At the photosphere, the density is so low that the gas is again transparent to light. – The hot convection cell tops radiate energy as a function of their temperature (5800 K). ...
Overview: The Sun The outer layers Photosphere: Visible Surface
... • Convection: transfer of energy through currents • Dark-colored areas => cooler gas • Light-colored areas => hotter gas ...
... • Convection: transfer of energy through currents • Dark-colored areas => cooler gas • Light-colored areas => hotter gas ...
Review-Sheet-sun-solar-system-galaxies-and-cosmology-fall
... 1. What are the three layers of the sun’s interior? What part is responsible for fusion? 2. What are the three layers of the Sun’s atmosphere? Be able to describe them briefly, such as lowest layer, the visible surface, etc… 3. What is the solar wind? What happens when the solar wind gets trapped in ...
... 1. What are the three layers of the sun’s interior? What part is responsible for fusion? 2. What are the three layers of the Sun’s atmosphere? Be able to describe them briefly, such as lowest layer, the visible surface, etc… 3. What is the solar wind? What happens when the solar wind gets trapped in ...
The Sun - rosedalegrade9astronomy
... – Is our nearest star. It is 5 billion years old. – It will last another 5 billion years – Has the mass of more than 300 000 Earths – So big that gravity forces everything together so tight that there are nuclear reactions and a great amount of heat. -Hydrogen atoms are squashed together to form hel ...
... – Is our nearest star. It is 5 billion years old. – It will last another 5 billion years – Has the mass of more than 300 000 Earths – So big that gravity forces everything together so tight that there are nuclear reactions and a great amount of heat. -Hydrogen atoms are squashed together to form hel ...
The Sun`s Crowning Glory - Max-Planck
... the universe is in the plasma state. Sunspots Regions that are around 1,500 degrees Celsius cooler than the undisturbed visible solar surface (photosphere). Owing to the low temperature, they appear dark in contrast. Sunspots are caused by disturbances in the solar magnetic field. They often appear ...
... the universe is in the plasma state. Sunspots Regions that are around 1,500 degrees Celsius cooler than the undisturbed visible solar surface (photosphere). Owing to the low temperature, they appear dark in contrast. Sunspots are caused by disturbances in the solar magnetic field. They often appear ...
Unit 9 Day 9 Notes
... Tiny grains of condensed material began to accumulate and merge to form larger bodies then collide and stick together Eventually these bodies reached hundreds of kilometers in diameter and are called planetesimals that continued to grow through collisions with other objects ...
... Tiny grains of condensed material began to accumulate and merge to form larger bodies then collide and stick together Eventually these bodies reached hundreds of kilometers in diameter and are called planetesimals that continued to grow through collisions with other objects ...
Foundation 1 - Discovering Astronomy
... Outer Layers of the Sun’s Atmosphere • Photosphere - the 5800 K layer we see • Chromosphere - the red layer observed using a hydrogen filter at a million degrees • Corona - the incredibly thin outer atmosphere at millions of degrees ...
... Outer Layers of the Sun’s Atmosphere • Photosphere - the 5800 K layer we see • Chromosphere - the red layer observed using a hydrogen filter at a million degrees • Corona - the incredibly thin outer atmosphere at millions of degrees ...
Name Date_____________________________________
... The Sun is the largest object in our (1) ______________________________________________________. Its (2)____________________________ controls the motions of the planets. The center of the Sun is very dense. The high temperature at its center causes the solar interior to be (3) ______________________ ...
... The Sun is the largest object in our (1) ______________________________________________________. Its (2)____________________________ controls the motions of the planets. The center of the Sun is very dense. The high temperature at its center causes the solar interior to be (3) ______________________ ...
No Slide Title
... • It is a huge ball of hot gases (mostly hydrogen and helium). • It is a star (an object that produces its own energy). ...
... • It is a huge ball of hot gases (mostly hydrogen and helium). • It is a star (an object that produces its own energy). ...
29.1-homework - Stout Middle School
... The Sun is the largest object in our (1) ______________________________________________________. Its (2)____________________________ controls the motions of the planets. The center of the Sun is very dense. The high temperature at its center causes the solar interior to be (3) ______________________ ...
... The Sun is the largest object in our (1) ______________________________________________________. Its (2)____________________________ controls the motions of the planets. The center of the Sun is very dense. The high temperature at its center causes the solar interior to be (3) ______________________ ...
Astronomy Solar System Formation Sun and Stellar Evolution
... 6. Identify major characteristics of each layer and what processes are taking place in each layer. 7. Describe how temperature changes as you move from the core to the corona. 8. Identify and explain characteristics of an active Sun a. Granulation b. Sunspots c. Filaments d. Prominences e. Flares f. ...
... 6. Identify major characteristics of each layer and what processes are taking place in each layer. 7. Describe how temperature changes as you move from the core to the corona. 8. Identify and explain characteristics of an active Sun a. Granulation b. Sunspots c. Filaments d. Prominences e. Flares f. ...
The Sun - TeacherWeb
... – This energy and light released from the sun takes 8 minutes to reach us ...
... – This energy and light released from the sun takes 8 minutes to reach us ...
Stars - Independence High School
... • Reaches Earth at 400 km/s • Particles collide with atmospheric gases to form auroras ...
... • Reaches Earth at 400 km/s • Particles collide with atmospheric gases to form auroras ...
PLANETARY ATMOSPHERES HOMEWORK
... visible light produced in the photosphere (give your answer in minutes) x-rays from a flare (give your answer in minutes) Solar wind particles traveling at 400 km/s (give your answer in days) A CME moving with a velocity of 1500 km/sec (give your answer in days) A jet aircraft traveling at 220 m/s ( ...
... visible light produced in the photosphere (give your answer in minutes) x-rays from a flare (give your answer in minutes) Solar wind particles traveling at 400 km/s (give your answer in days) A CME moving with a velocity of 1500 km/sec (give your answer in days) A jet aircraft traveling at 220 m/s ( ...
The Sun
... When the Coronal mass ejection reaches the Earth it may disrupt the Earth's magnetosphere, compressing it on the day side and extending the night-side magnetic tail. This process can cause particularly strong aurora in large regions around Earth's magnetic poles. These are also known as the Northern ...
... When the Coronal mass ejection reaches the Earth it may disrupt the Earth's magnetosphere, compressing it on the day side and extending the night-side magnetic tail. This process can cause particularly strong aurora in large regions around Earth's magnetic poles. These are also known as the Northern ...
File
... 2. _______ - thin spikes of matter C. ___________ 1. The upper ___________ of the Sun 2. During a total eclipse, __________ lines appear 3. __ ________ K !! Seems to contradict common sense.. Energy transferred as magnetism & ”sound” 4. Corona can be studied using _______ D. The Solar Wind 1. The st ...
... 2. _______ - thin spikes of matter C. ___________ 1. The upper ___________ of the Sun 2. During a total eclipse, __________ lines appear 3. __ ________ K !! Seems to contradict common sense.. Energy transferred as magnetism & ”sound” 4. Corona can be studied using _______ D. The Solar Wind 1. The st ...
Our Star, the Sun Chapter Eighteen Guiding Questions
... The corona ejects mass into space to form the solar wind ...
... The corona ejects mass into space to form the 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.