Standard 1 Objectives 1 and 2 Workbook
... Standard 1: Students will understand the scientific evidence that supports theories that explain how the universe and the solar system developed. They will compare Earth to other objects in the solar system. Objective 1: Describe both the big bang theory of universe formation and the nebular theory ...
... Standard 1: Students will understand the scientific evidence that supports theories that explain how the universe and the solar system developed. They will compare Earth to other objects in the solar system. Objective 1: Describe both the big bang theory of universe formation and the nebular theory ...
Document
... How did the Solar System Form: Jovian Planets. • Formation of the Jovian or gas-giant planets is a little less clear with a weaker consensus among scientists as to a party-line theory. – 1. These planets simply grew large or massive enough that their gravitational fields pulled large masses of gas ...
... How did the Solar System Form: Jovian Planets. • Formation of the Jovian or gas-giant planets is a little less clear with a weaker consensus among scientists as to a party-line theory. – 1. These planets simply grew large or massive enough that their gravitational fields pulled large masses of gas ...
here - GLORIA Project
... The auroral are phenomenon low luminous, so it can be observed only at night. The weak auroras have brightness similar to the Milky Way one, while the brightest can come to have luminosity similar to the full moon. Due to the fact that auroras are visible only in the circumpolar regions, they shall ...
... The auroral are phenomenon low luminous, so it can be observed only at night. The weak auroras have brightness similar to the Milky Way one, while the brightest can come to have luminosity similar to the full moon. Due to the fact that auroras are visible only in the circumpolar regions, they shall ...
3D View of a Comet`s Neighborhood
... halo develop a slight positive potential, which new electrons must overcome to escape the vicinity of the comet. The po- ...
... halo develop a slight positive potential, which new electrons must overcome to escape the vicinity of the comet. The po- ...
Lecture 9
... large, low-density cloud of dusty gas. Such gas clouds can be seen in our Milky Way and other galaxies today. ASTR111 Lecture 9 ...
... large, low-density cloud of dusty gas. Such gas clouds can be seen in our Milky Way and other galaxies today. ASTR111 Lecture 9 ...
Chapter 9 Life and Times on the Main Sequence
... • The assumption that the Sun was formed from a homogenous mixture of gases is motivated by the strong convection expected in the protostar during collapse to the main sequence. • The surface abundances are then assumed to have been undisturbed in the subsequent evolution, so that present surface ab ...
... • The assumption that the Sun was formed from a homogenous mixture of gases is motivated by the strong convection expected in the protostar during collapse to the main sequence. • The surface abundances are then assumed to have been undisturbed in the subsequent evolution, so that present surface ab ...
Explore the Galaxy - Museum of Science
... 1) The activity sheet and answ er key (13 total pages) 2) The "p lanet card s" referred to in the activity (2 pages) A m ore d etailed d escrip tion of this activity can be fou nd at the end of this gu id e. ...
... 1) The activity sheet and answ er key (13 total pages) 2) The "p lanet card s" referred to in the activity (2 pages) A m ore d etailed d escrip tion of this activity can be fou nd at the end of this gu id e. ...
welsch_harvey_20100526
... and can extend through the photosphere into the corona, coupling the Sun's interior with its outer atmosphere. Hence, measurements of magnetic fields at the photosphere can provide insights into magnetic evolution both in the interior and the outer atmosphere. While maps of the photospheric magnetic ...
... and can extend through the photosphere into the corona, coupling the Sun's interior with its outer atmosphere. Hence, measurements of magnetic fields at the photosphere can provide insights into magnetic evolution both in the interior and the outer atmosphere. While maps of the photospheric magnetic ...
Homework #4 (Ch. 16)
... areas of concentrated magnetic field repel hot material trying to rise up from the Sun’s interior, so the section of the Sun underneath the knot cools off and darkens. Flares, by contrast, are areas where large amounts of energy are released in a short amount of time. Their origin is mysterious, but ...
... areas of concentrated magnetic field repel hot material trying to rise up from the Sun’s interior, so the section of the Sun underneath the knot cools off and darkens. Flares, by contrast, are areas where large amounts of energy are released in a short amount of time. Their origin is mysterious, but ...
astro-ph/0502206 PDF
... a. Solar magnetic fields may determine the effectiveness of the sorting process. A recent survey [7] found iron-rich surfaces of stars during periods of low magnetic activity, like the Sun’s "Maunder minimum" that accompanied the "Little Ice Age" in Europe. b. Magnetic fields that penetrate the sola ...
... a. Solar magnetic fields may determine the effectiveness of the sorting process. A recent survey [7] found iron-rich surfaces of stars during periods of low magnetic activity, like the Sun’s "Maunder minimum" that accompanied the "Little Ice Age" in Europe. b. Magnetic fields that penetrate the sola ...
Geomagnetic Storms - Thought Leadership
... This document is intended for general information purposes only and should not be construed as advice or opinions on any specific facts or circumstances. The comments in this summary are based upon Aon Benfield’s preliminary analysis of publicly available information. The content of this document is ...
... This document is intended for general information purposes only and should not be construed as advice or opinions on any specific facts or circumstances. The comments in this summary are based upon Aon Benfield’s preliminary analysis of publicly available information. The content of this document is ...
Enhanced temperature regions in the polar zones of the Sun
... the receiver is sufficient for 0.1 sfu resolution. In the temperature scale this corresponds to better than 100 K, and it is limited by short term changes in the atmospheric attenuation. Solar maps are measured by scanning the solar disk in right ascension and by changing the declination in small st ...
... the receiver is sufficient for 0.1 sfu resolution. In the temperature scale this corresponds to better than 100 K, and it is limited by short term changes in the atmospheric attenuation. Solar maps are measured by scanning the solar disk in right ascension and by changing the declination in small st ...
AMPTE: NOTES ON THE INITIAL ... WORK IN PROGRESS _ _ _ _ _... _
... The West German spacecraft, the Ion Release Module (lRM), has the job of releasing canisters of barium and lithium (neither of which is known to occur naturally in space in appreciable quantities), which become the ions to be studied. The British spacecraft, the United Kingdom Subsatellite, monitors ...
... The West German spacecraft, the Ion Release Module (lRM), has the job of releasing canisters of barium and lithium (neither of which is known to occur naturally in space in appreciable quantities), which become the ions to be studied. The British spacecraft, the United Kingdom Subsatellite, monitors ...
observatory - Science Presenters Central
... Features of the ACTIVE Sun: The Sun’s atmosphere is periodically changed by its magnetic fields, and the most common features of these changes are sunspots. These are areas of the photosphere that appear dark because they are cooler than the rest of the Sun’s lower atmosphere. Most of the time, the ...
... Features of the ACTIVE Sun: The Sun’s atmosphere is periodically changed by its magnetic fields, and the most common features of these changes are sunspots. These are areas of the photosphere that appear dark because they are cooler than the rest of the Sun’s lower atmosphere. Most of the time, the ...
Presentation - Harvard-Smithsonian Center for Astrophysics
... Suggests that high T plasma, 6.8 K (dex) is anchored close to the stellar surface reminiscent of low-lying coronal loops… ...
... Suggests that high T plasma, 6.8 K (dex) is anchored close to the stellar surface reminiscent of low-lying coronal loops… ...
3D Motion Analysis from 2D Monochromatic Images of a Solar
... The Sun is a strong source of constantly changing magnetic fields. The ionized plasma is a rope in a constant tug-of-war match between changing magnetic fields and thermal pressures. Like most tug-of-war matches, they easily become violent. This leads to instabilities, often resulting in prominences ...
... The Sun is a strong source of constantly changing magnetic fields. The ionized plasma is a rope in a constant tug-of-war match between changing magnetic fields and thermal pressures. Like most tug-of-war matches, they easily become violent. This leads to instabilities, often resulting in prominences ...
Coronal magnetic topology and the production of solar impulsive
... field lines are rooted in AR10154, while closed field lines dominate above AR10160. Therefore, it is necessary to examine the magnetic field configurations above the two ARs. We trace the coronal magnetic field lines, rooted in the two ARs and extended to 2.5 Rs , by applying the potential field sou ...
... field lines are rooted in AR10154, while closed field lines dominate above AR10160. Therefore, it is necessary to examine the magnetic field configurations above the two ARs. We trace the coronal magnetic field lines, rooted in the two ARs and extended to 2.5 Rs , by applying the potential field sou ...
A Solar Polar Imager Concept - The National Academies of
... depth from SOHO/MDI data. A region of large velocity shear can be seen at about 0.7 RSun; it is this shear, at the base of the convection zone (tachocline) that is now thought to drive the largescale solar dynamo. Observations from the Solar Optical Telescope on Hinode during the periods of the high ...
... depth from SOHO/MDI data. A region of large velocity shear can be seen at about 0.7 RSun; it is this shear, at the base of the convection zone (tachocline) that is now thought to drive the largescale solar dynamo. Observations from the Solar Optical Telescope on Hinode during the periods of the high ...
Lecture 5: Solar System Formation Theories
... accretion rate and gravitational accretion rate small. o By time inner planetesimals were formed and had significant gravitational fields, the nebula had been cleared out by the solar wind. o Then no nebular gas then present to capture an elementary atmosphere. ...
... accretion rate and gravitational accretion rate small. o By time inner planetesimals were formed and had significant gravitational fields, the nebula had been cleared out by the solar wind. o Then no nebular gas then present to capture an elementary atmosphere. ...
background_items_1_3 (1)
... SRRR group is composed by two kinds of participants: producers and evaluators. The first are manufacturers, active in the solar-mirror market; the latter are scientists/technicians, highly experienced in reflectance measurements, working in one of the participating research institutes. Producers sent ...
... SRRR group is composed by two kinds of participants: producers and evaluators. The first are manufacturers, active in the solar-mirror market; the latter are scientists/technicians, highly experienced in reflectance measurements, working in one of the participating research institutes. Producers sent ...
Coronal Polarization Measurements and
... small dust particles in the ecliptic plane results in the Fraunhofer (or F-) corona, named for the photospheric Fraunhofer absorption lines it displays (Golub and Pasachoff, 1997, p. 3-6). Often the first task of a scientist studying coronal light is to separate the contributions from each of these ...
... small dust particles in the ecliptic plane results in the Fraunhofer (or F-) corona, named for the photospheric Fraunhofer absorption lines it displays (Golub and Pasachoff, 1997, p. 3-6). Often the first task of a scientist studying coronal light is to separate the contributions from each of these ...
Conceptual steps towards exploring the fundamental nature of our Sun
... All aspects of solar activity (Ellerman Bombs, Bright Points, flares, particle acceleration etc.) are self-similar and their statistical behavior follows well-defined power laws. This last point reinforces the belief that the solar atmosphere is coupled, through the magnetic field, with the convecti ...
... All aspects of solar activity (Ellerman Bombs, Bright Points, flares, particle acceleration etc.) are self-similar and their statistical behavior follows well-defined power laws. This last point reinforces the belief that the solar atmosphere is coupled, through the magnetic field, with the convecti ...
May - RASC Hamilton
... traveled 950 kilometres from Toronto to Ottawa, Illinois to find clear skies, and produced the image on the front cover of Orbit this month. It is one of the most beautiful pictures of a lunar eclipse I’ve seen, and it captures perfectly the sort of view I’d expect through a wide field eyepiece or a ...
... traveled 950 kilometres from Toronto to Ottawa, Illinois to find clear skies, and produced the image on the front cover of Orbit this month. It is one of the most beautiful pictures of a lunar eclipse I’ve seen, and it captures perfectly the sort of view I’d expect through a wide field eyepiece or a ...
Solar System - CW Perry School
... This is an important question, and one that is difficult for scientists to understand. After all, the creation of our Solar System took place billions of years before there were any people around to witness it. Our own evolution is tied closely to the evolution of the Solar System. Thus, without und ...
... This is an important question, and one that is difficult for scientists to understand. After all, the creation of our Solar System took place billions of years before there were any people around to witness it. Our own evolution is tied closely to the evolution of the Solar System. Thus, without und ...
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.