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 ...
Propagation of cosmic rays in the solar wind
... first reportedby Forbu.sh[1954] and is now known to consistof a cyclic, elevenyear, solar-cycle variation upon which are superposedshorter-term irregular fluctuations (called Forbush decreases). This modulation is strongest at low energies.Initially, a number of authors consideredthe possibility of ...
... first reportedby Forbu.sh[1954] and is now known to consistof a cyclic, elevenyear, solar-cycle variation upon which are superposedshorter-term irregular fluctuations (called Forbush decreases). This modulation is strongest at low energies.Initially, a number of authors consideredthe possibility of ...
Explore the Galaxy - Museum of Science
... Potential Pitfalls/Things to Look Out For 1) The Y axis for grap h 1 extend s beyond zero into negative nu m bers. Rem ind stu d ents to w atch ou t for these negative nu m bers w hen grap hing. 2) Since stu d ents are instru cted to m ix u p the card s betw een d ata collection, rem ind them to d o ...
... Potential Pitfalls/Things to Look Out For 1) The Y axis for grap h 1 extend s beyond zero into negative nu m bers. Rem ind stu d ents to w atch ou t for these negative nu m bers w hen grap hing. 2) Since stu d ents are instru cted to m ix u p the card s betw een d ata collection, rem ind them to d o ...
A diffusive description of the focused transport of solar energetic
... motion around the large-scale magnetic field lines. The small superposed irregularities interact with the gyrating particles in such a way that the first adiabatic invariant (the magnetic moment) is not conserved, leading to a scattering of the pitch angle, θ (angle between the velocity vector u of ...
... motion around the large-scale magnetic field lines. The small superposed irregularities interact with the gyrating particles in such a way that the first adiabatic invariant (the magnetic moment) is not conserved, leading to a scattering of the pitch angle, θ (angle between the velocity vector u of ...
CME - ASU
... For weak CMEs at .5 AU, M=.25*Earth's is sufficient for only 1 Earth radius standoff. For strong CMEs, M = 2*Earth's, so cannot be generated by tidally locked Earth size and mass exoplanets ...
... For weak CMEs at .5 AU, M=.25*Earth's is sufficient for only 1 Earth radius standoff. For strong CMEs, M = 2*Earth's, so cannot be generated by tidally locked Earth size and mass exoplanets ...
Plasma: the 4th State of Matter and a Path to Fusion Energy use in
... • Examples of plasmas on Earth: – Lightning – Neon and fluorescent lights – Laboratory experiments ...
... • Examples of plasmas on Earth: – Lightning – Neon and fluorescent lights – Laboratory experiments ...
Week 5 - OSU Astronomy
... Sun is in thermal equilibrium • Its temperature is not changing • Energy being radiated (lost) at surface is balanced by energy generated in interior • This means temperature is highest at center, coolest at surface – if temperature were not high at center, surface would cool off ...
... Sun is in thermal equilibrium • Its temperature is not changing • Energy being radiated (lost) at surface is balanced by energy generated in interior • This means temperature is highest at center, coolest at surface – if temperature were not high at center, surface would cool off ...
Diffusion of Open Magnetic Flux and Its Consequences
... It is important to treat the open flux and the solar wind as a coupled problem. Open flux can be considered to be open only if there is a flo w of solar wind along it that is capable of carrying the open flux out into th e ...
... It is important to treat the open flux and the solar wind as a coupled problem. Open flux can be considered to be open only if there is a flo w of solar wind along it that is capable of carrying the open flux out into th e ...
Neutron Star Formation
... Becomes so High that: Iron dissociates into alpha particles Electrons capture onto protons Core collapses nearly at freefall! ...
... Becomes so High that: Iron dissociates into alpha particles Electrons capture onto protons Core collapses nearly at freefall! ...
bution of Solar Proton Events Affecting the Earth E
... transport of SEPs. It is very difficult to analytically solve the multidimensional transport equation; consequently, numerical calculations are usually adopted (e.g., [2, 3]). Recently, [3] investigated the effects of particle source characteristics on SEP observations at 1 AU and found that the per ...
... transport of SEPs. It is very difficult to analytically solve the multidimensional transport equation; consequently, numerical calculations are usually adopted (e.g., [2, 3]). Recently, [3] investigated the effects of particle source characteristics on SEP observations at 1 AU and found that the per ...
nearest star
... There is much that is new on and under the Sun in the intervening years, and it is a pleasure to be able to describe it here. One of us (JMP) got his start in solar astronomy from both the distinguished scientists who were just listed. Donald Menzel took him, as a Harvard first-year student, to a tot ...
... There is much that is new on and under the Sun in the intervening years, and it is a pleasure to be able to describe it here. One of us (JMP) got his start in solar astronomy from both the distinguished scientists who were just listed. Donald Menzel took him, as a Harvard first-year student, to a tot ...
Solutions - Physics @ IUPUI
... a) none b) emission c) continuous d) absorption 22) Where on the sun could you land? a) bottom of the photosphere b) core c) coronal hole d) no where 23) How dense is the sun? a) about as dense as air b) about as dense as water c) about as dense as lead d) more dense than any material on the earth! ...
... a) none b) emission c) continuous d) absorption 22) Where on the sun could you land? a) bottom of the photosphere b) core c) coronal hole d) no where 23) How dense is the sun? a) about as dense as air b) about as dense as water c) about as dense as lead d) more dense than any material on the earth! ...
Conceptual Test PowerPoint Chapter 2 Astronomy Today, 5th
... he was unable to observe which of the following? ...
... he was unable to observe which of the following? ...
What`s important to know about planet Mercury?
... charged particles similarly to how Earth does, creating a "hot flow anomaly" that has been observed on other planets. Because particles flowing from the Sun don't come uniformly, they can 7. Mercury is hard to spot in the sky, but has get turbulent when they encounter a planet's been known for mille ...
... charged particles similarly to how Earth does, creating a "hot flow anomaly" that has been observed on other planets. Because particles flowing from the Sun don't come uniformly, they can 7. Mercury is hard to spot in the sky, but has get turbulent when they encounter a planet's been known for mille ...
pres
... 2. How does the Solar System work? 2.1 From the Sun to the edge of the Solar System Study the plasma and magnetic field environment around the Earth and around Jupiter, over the Sun’s poles, and out to the heliosphere where the solar wind meets the interstellar medium. 2.2 The giant planets and thei ...
... 2. How does the Solar System work? 2.1 From the Sun to the edge of the Solar System Study the plasma and magnetic field environment around the Earth and around Jupiter, over the Sun’s poles, and out to the heliosphere where the solar wind meets the interstellar medium. 2.2 The giant planets and thei ...
Document
... 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 to their “cores”. – 2. They formed from instabilities in the cool outer regions of the solar nebula, mimick ...
... 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 to their “cores”. – 2. They formed from instabilities in the cool outer regions of the solar nebula, mimick ...
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 ...
Protecting planets from their stars
... A magnetic field has not yet been observed on extrasolar planets. Detection of radio emission would not only constrain local characteristics of the stellar wind, but would also demonstrate that exoplanets are magnetized. Fortunately, there may be other ways to probe exoplanetary magnetic fields, in ...
... A magnetic field has not yet been observed on extrasolar planets. Detection of radio emission would not only constrain local characteristics of the stellar wind, but would also demonstrate that exoplanets are magnetized. Fortunately, there may be other ways to probe exoplanetary magnetic fields, in ...
observatory - Science Presenters Central
... last for a few hours to months. Some can escape the magnetic fields that hold them in and go out into space. Violent, eruptive events on the Sun, called solar flares, also send out huge amounts of particles like X-rays and ultraviolet radiation. At the maximum of the sunspot cycle there are 1,100 fl ...
... last for a few hours to months. Some can escape the magnetic fields that hold them in and go out into space. Violent, eruptive events on the Sun, called solar flares, also send out huge amounts of particles like X-rays and ultraviolet radiation. At the maximum of the sunspot cycle there are 1,100 fl ...
Using gamma-rays to probe the clumped structure of stellar winds
... ∆Iγ = Ib σn∆z = Ib σn∆Nc h. Figure 2: 3D-plot with the light curve and the specBut by standard statistics for finite contributions tral energy distribution resulting from a from a discrete number ∆Nc , the variance of this jet-clump interaction. The main param- emission is eters adopted are indicate ...
... ∆Iγ = Ib σn∆z = Ib σn∆Nc h. Figure 2: 3D-plot with the light curve and the specBut by standard statistics for finite contributions tral energy distribution resulting from a from a discrete number ∆Nc , the variance of this jet-clump interaction. The main param- emission is eters adopted are indicate ...
Discrimination of exoplanetary and stellar radio flux
... density variations of a factor of two in the decimetric and centimetric wavelength range with 27 days period (due to the solar rotation). It is frequently circularly polarized. Noise storms During solar maximum, noise storms frequently occur (about 10% of the time). The typical duration is between a ...
... density variations of a factor of two in the decimetric and centimetric wavelength range with 27 days period (due to the solar rotation). It is frequently circularly polarized. Noise storms During solar maximum, noise storms frequently occur (about 10% of the time). The typical duration is between a ...
Sample pages 2 PDF
... it in fact presents a zone of gravitational equilibrium between the Sun and Jupiter, which existed during the process of simultaneous growing. The location of this zone was not fixed. The Sun’s gravitational pull grew more quickly than that of Jupiter, and therefore the gravitational equilibrium zone ...
... it in fact presents a zone of gravitational equilibrium between the Sun and Jupiter, which existed during the process of simultaneous growing. The location of this zone was not fixed. The Sun’s gravitational pull grew more quickly than that of Jupiter, and therefore the gravitational equilibrium zone ...
PowerPoint - Astronomy at Swarthmore College
... Figure 4 - Phase-folded light curves of 1 Ori C. Open circles represent the excess C IV 1548, 1551 Å equivalent width (left axis) taken from Walborn & Nichols (1994) and phased to the ephemeris of Stahl et al. (1996) with period 15.422 days and MJD0 = 48832.50. Maximum C IV absorption occurs near p ...
... Figure 4 - Phase-folded light curves of 1 Ori C. Open circles represent the excess C IV 1548, 1551 Å equivalent width (left axis) taken from Walborn & Nichols (1994) and phased to the ephemeris of Stahl et al. (1996) with period 15.422 days and MJD0 = 48832.50. Maximum C IV absorption occurs near p ...
spherical winds – spherical accretion
... There is one very general property of a steady – state wind model: in the deep stellar interior the star should be in a hydrostatic equilibrium, i.e. we should have v ≪ vs , where vs is speed of sound. At very large distance from a star we expect the flow to escape from gravitational potential, and ...
... There is one very general property of a steady – state wind model: in the deep stellar interior the star should be in a hydrostatic equilibrium, i.e. we should have v ≪ vs , where vs is speed of sound. At very large distance from a star we expect the flow to escape from gravitational potential, and ...
Solar wind
The solar wind is a stream of charged particles released from the upper atmosphere of the Sun. This plasma consists of mostly electrons, protons and alpha particles with energies usually between 1.5 and 10 keV; embedded in the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar longitude. Its particles can escape the Sun's gravity because of their high energy, from the high temperature of the corona and magnetic, electrical and electromagnetic phenomena in it.The solar wind flows outward supersonically to great distances, filling a region known as the heliosphere, an enormous bubble-like volume surrounded by the interstellar medium. Other related phenomena include the aurora (northern and southern lights), the plasma tails of comets that always point away from the Sun, and geomagnetic storms that can change the direction of magnetic field lines and create strong currents in power grids on Earth.