ppt
... •Appearance Oscillation can be seen in tagged mode with low background Measure θ23 •More work needed to see if 2nd max can be seen sufficiently well to go beyond osc. to see solar interference CP violation Heirarchy effects. Energy close to Fermi motion limit— can one use C and p or only p? ...
... •Appearance Oscillation can be seen in tagged mode with low background Measure θ23 •More work needed to see if 2nd max can be seen sufficiently well to go beyond osc. to see solar interference CP violation Heirarchy effects. Energy close to Fermi motion limit— can one use C and p or only p? ...
Many-body Physics in Neutrino Detection and Dark Matter Searches
... If yes, reporters are neutrinos. Photons are historians. ...
... If yes, reporters are neutrinos. Photons are historians. ...
galactic cosmic radiation and solar energetic particles
... Figure 6-5. The "anomaly" can be seen by comparing this spectra with that of the previous solar minima, the upper envelope of the low energy portion of the spectra shown in Figure 6-2. In a review of this anomalous component, Gloeckler [1979] noted that the helium spectra above - 2 MeV/nucleon was r ...
... Figure 6-5. The "anomaly" can be seen by comparing this spectra with that of the previous solar minima, the upper envelope of the low energy portion of the spectra shown in Figure 6-2. In a review of this anomalous component, Gloeckler [1979] noted that the helium spectra above - 2 MeV/nucleon was r ...
PDF
... neutrino mass, the standard model is in splendid agreement with all confirmed measurements. However, it is also clear that particle physics is playing the game with much less than a full deck of ―cards‖ because of the apparent existence of dark matter and dark energy, which, respectively, constitute ...
... neutrino mass, the standard model is in splendid agreement with all confirmed measurements. However, it is also clear that particle physics is playing the game with much less than a full deck of ―cards‖ because of the apparent existence of dark matter and dark energy, which, respectively, constitute ...
The Electromagnetic Spectrum
... Hydrogen fusion to Helium • The sun’s core is 10 million °K. • At this temperature, hydrogen nuclei fuse into helium • Huge amounts of energy are released. ...
... Hydrogen fusion to Helium • The sun’s core is 10 million °K. • At this temperature, hydrogen nuclei fuse into helium • Huge amounts of energy are released. ...
scholer-shocks
... Solar System Solar wind speed 400 – 600 km/sec Alfven speed about 40 km/sec: There have to be shocks ...
... Solar System Solar wind speed 400 – 600 km/sec Alfven speed about 40 km/sec: There have to be shocks ...
Sec 29.1 - Highland High School
... surface. It has an average temperature of 5800 K and is about 400 km thick 2.Chromosphere – above the photosphere, 2500 km thick and has a temperature of nearly 30,000 K visible only during a solar eclipse. 3.Corona - outermost layer extends several million kilometers from the outside edge of the ch ...
... surface. It has an average temperature of 5800 K and is about 400 km thick 2.Chromosphere – above the photosphere, 2500 km thick and has a temperature of nearly 30,000 K visible only during a solar eclipse. 3.Corona - outermost layer extends several million kilometers from the outside edge of the ch ...
teacher resource - Michigan Science Center
... A solar flare is a sudden, rapid, and intense variation in brightness on the sun’s surface. A solar flare occurs when magnetic energy has built up in the sun’s atmosphere and is suddenly released. The amount of energy released is equivalent to 100-megaton hydrogen bombs exploding at the same time! T ...
... A solar flare is a sudden, rapid, and intense variation in brightness on the sun’s surface. A solar flare occurs when magnetic energy has built up in the sun’s atmosphere and is suddenly released. The amount of energy released is equivalent to 100-megaton hydrogen bombs exploding at the same time! T ...
Full text - terrapub
... The ASPERA ion composition spectrometer made it possible to measure the distribution of different ion species. It was shown (Lundin et al., 1990; Norberg et al., 1993) that the inner magnetosphere of Mars is filled not only by O+-ions but contains also a substantial admixture of molecular ions (O2+, ...
... The ASPERA ion composition spectrometer made it possible to measure the distribution of different ion species. It was shown (Lundin et al., 1990; Norberg et al., 1993) that the inner magnetosphere of Mars is filled not only by O+-ions but contains also a substantial admixture of molecular ions (O2+, ...
Comets
... 1. What are the characteristics of comets? Like a dirty snowball. Nucleus – center solid part of the comet Coma – fuzzy cloud of vaporized gases around the nucleus Tail – stream of dust and gases; always points away from sun 2. Where are most asteroids found? Between the orbits of Mars and Jupiter i ...
... 1. What are the characteristics of comets? Like a dirty snowball. Nucleus – center solid part of the comet Coma – fuzzy cloud of vaporized gases around the nucleus Tail – stream of dust and gases; always points away from sun 2. Where are most asteroids found? Between the orbits of Mars and Jupiter i ...
The abundance of 26Al-rich planetary systems in the Galaxy
... Iron-60 (τ = 3.7 Myr), which decays onto 60 Ni, is another key short-lived radionuclide whose origin is often discussed in conjunction with that of 26 Al (see below). Because mass-independent nickel isotopic anomalies are ubiquitous in CAIs (Birck & Lugmair 1988), the search for the earlier presence ...
... Iron-60 (τ = 3.7 Myr), which decays onto 60 Ni, is another key short-lived radionuclide whose origin is often discussed in conjunction with that of 26 Al (see below). Because mass-independent nickel isotopic anomalies are ubiquitous in CAIs (Birck & Lugmair 1988), the search for the earlier presence ...
spicam on mars express:the atmosphere of mars from top to bottom
... (Figure adopted from Hechler and Yanes, 1999.) Because the CO2 cross-section presents an enormous dynamic range in the UV, the CO2 absorption may be detected already at an altitude of 150 km. For decreasing tangential heights, the CO2 manifests itself (figure 6) by a sharp cut-off which increases in ...
... (Figure adopted from Hechler and Yanes, 1999.) Because the CO2 cross-section presents an enormous dynamic range in the UV, the CO2 absorption may be detected already at an altitude of 150 km. For decreasing tangential heights, the CO2 manifests itself (figure 6) by a sharp cut-off which increases in ...
A breath of oxygen for the Sun
... hydrodynamical model of the solar atmosphere, while traditional models are 1D. The model allows to derive the 3D temperature structure and velocity field in the solar surface layers where the spectral lines are formed. The oxygen abundance they found are in much better agreement with helioseismology ...
... hydrodynamical model of the solar atmosphere, while traditional models are 1D. The model allows to derive the 3D temperature structure and velocity field in the solar surface layers where the spectral lines are formed. The oxygen abundance they found are in much better agreement with helioseismology ...
SR - SwRI IMAGE HomePage
... Most of these studies are made possible by the new viewing perspective that results from the precession of the IMAGE orbit to middle and low latitudes. Open data policy encourages collaborations and new initiatives from non-team members (Guest Investigators and others). ...
... Most of these studies are made possible by the new viewing perspective that results from the precession of the IMAGE orbit to middle and low latitudes. Open data policy encourages collaborations and new initiatives from non-team members (Guest Investigators and others). ...
Return both exam and scantron sheet when you
... 37. When does the intensity of the solar wind have the highest value? (a) During the solar activity maximum as measured by the number of sunspots. (b) During the solar activity minimum as measured by the number of sunspots. (c) The intensity of the solar wind does not depend on the solar activity. 3 ...
... 37. When does the intensity of the solar wind have the highest value? (a) During the solar activity maximum as measured by the number of sunspots. (b) During the solar activity minimum as measured by the number of sunspots. (c) The intensity of the solar wind does not depend on the solar activity. 3 ...
Advanced Composition Explorer
Advanced Composition Explorer (ACE) is a NASA Explorers program Solar and space exploration mission to study matter comprising energetic particles from the solar wind, the interplanetary medium, and other sources. Real-time data from ACE is used by the NOAA Space Weather Prediction Center to improve forecasts and warnings of solar storms. The ACE robotic spacecraft was launched August 25, 1997 and entered a Lissajous orbit close to the L1 Lagrangian point (which lies between the Sun and the Earth at a distance of some 1.5 million km from the latter) on December 12, 1997. The spacecraft is currently operating at that orbit. Because ACE is in a non-Keplerian orbit, and has regular station-keeping maneuvers, the orbital parameters at right are only approximate. The spacecraft is still in generally good condition in 2015, and is projected to have enough fuel to maintain its orbit until 2024. NASA Goddard Space Flight Center managed the development and integration of the ACE spacecraft.