'Coronal holes' presentation slideshows

G3 - RADIO WAVE PROPAGATION [3 Exam Questions - 3 Groups]

G3 - RADIO WAVE PROPAGATION [3 Exam Questions - 3 Groups] . G3A Sunspots and solar radiation; ionospheric disturbances; propagation forecasting and indices G3B Maximum Usable Frequency; Lowest Usable Frequency; propagation "hops"

1.2k views • 102 slides

G3 - RADIO WAVE PROPAGATION [3 Exam Questions -- 3 Groups]

G3 - RADIO WAVE PROPAGATION [3 Exam Questions -- 3 Groups]. G3A - Sunspots and solar radiation; ionospheric disturbances; propagation forecasting and indices G3B - Maximum Usable Frequency; Lowest Usable Frequency; propagation

1.25k views • 92 slides

Solar Wind Origin & Heating 1

Solar Wind Origin & Heating 1. Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics. Logistics. Part 1: Observations. Part 2: Theory. 1. Photosphere: tip of the iceberg of the convection zone 2. Chromosphere: waves start to propagate and bump into the magnetic field

593 views • 46 slides

General Properties Internal Structure Solar Atmosphere Photosphere, chromosphere, and corona Surface Features and Magnet

622 views • 39 slides

Outline: Background Source regions & flux-tube expansion Heating above/below the critical point

485 views • 38 slides

Solar Drivers of Space Weather

Solar Drivers of Space Weather. Steven Hill NOAA/SEC June 14, 2007. Research Experience for Undergraduates. Energy and Power in Context. Outline. Overview of the Sun Interior Surface Corona Solar Drivers of Space Weather Coronal Holes Flares Coronal Mass Ejections (CMEs) Summary.

425 views • 32 slides

Ion Heating in the Solar Corona & Solar Wind

580 views • 27 slides

SUN

Solar mass: 1.98x10 33 gm. SUN. Solar radius: 6.96x10 10 cm. Quiescent Solar luminosity: 3.83x10 33 ergs/s. Mean Solar density: 1.410 gm cm -3. Earth-Sun distance: (1 AU): 1.5x10 13 cm. Visual magnitude of the Sun: -26.73. Solar constant: 0.1353 Watts cm -2.

504 views • 23 slides

ORIGIN OF THE SLOW SOLAR WIND

ORIGIN OF THE SLOW SOLAR WIND. K. Fujiki ? T. Ohmi, M. Kojima, M. Tokumaru Solar-Terrestrial Environment Laboratory, Nagoya University and K. Hakamada Department of Engineering Physics, Chubu University. Slow solar wind from a small equatorial coronal hole.

398 views • 22 slides

Working Group I: Solar

Working Group I: Solar. SESSIONS:. Filaments (Mon. afternoon + Tues morning) Activation through eruption Sub-surface (Wed. morning) Understanding the magnetic connection between sub-photospheric layers and the solar corona Coronal Holes (Thurs. morning)

321 views • 21 slides

Solar Wind Acceleration and Waves in the Corona Perspectives for a spectrometer on Solar C/Plan A

373 views • 20 slides

Solar wind turbulence from radio occultation data

Solar wind turbulence from radio occultation data. Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering & Electronics, Moscow, Russia Bird, M.K. Radio Astronomical Institute, Univ. Bonn, Bonn, Germany. TURBULENCE.

317 views • 19 slides

Coronal Holes Not As Well Behaved As We Thought

283 views • 19 slides

Kinematical Characterization of Intensity Fluctuations Observed in STEREO EUVI Images

Kinematical Characterization of Intensity Fluctuations Observed in STEREO EUVI Images. Katherine Baldwin Praxis, Inc. / NRL Guillermo Stenborg Interferometrics, Inc. / NRL Angelos Vourlidas, Russ Howard Naval Research Lab (NRL). Motivation - Robbrecht Waves.

239 views • 17 slides

The Sun as a Star

280 views • 16 slides

SLIDE SHOW 6. SOLAR WIND

ionized tail. dust tail. SLIDE SHOW 6. SOLAR WIND. Observations of comets suggested solar outflow (Biermann). Parker (1958) proposed supersonic expansion. Confirmed in 1960s by spacecraft measurements (Mariner 2, 1962). Slow wind (300 km/s) + Fast solar wind (700 km/s).

319 views • 12 slides

Flux Emergence Rate in Coronal Holes and in Adjacent Quiet-sun Regions

Flux Emergence Rate in Coronal Holes and in Adjacent Quiet-sun Regions. Valentyna Abramenko Big Bear Solar Observatory Lennard Fisk University of Michigan Vasyl Yurchyshyn Big Bear Solar Observatory. Abstract. 1. Coronal holes are regions where the open magnetic

233 views • 10 slides

Solar X-ray Imager (SXI) Current and Future Requirements

Solar X-ray Imager (SXI) Current and Future Requirements. Solar Causes and Effects... Operational Requirements Improvements for GOES-R+ Program Status Other Imaging. 22 May 2001 Steve Hill. Causes and. July 15-16, 2000. Electric Power Systems. Tripping. Voltage Variations.

270 views • 9 slides

Algorithm Preparation and Data Availability

for the SDO Investigations in the Context of the UK Virtual Observatory J.L. Culhane 1 , E.C. Auden 1 , Y.P. Elsworth 2 , R.A. Harrison 3 , M.J. Thompson 4. SDO Data on the Grid

133 views • 1 slides

Solar and Stellar Winds

Comet Hale Bopp. Dust tail. Ion tail. Coronal hole. Closed loops. Velocity. Density. Closed loops. Coronal hole. 1991 Solar Eclipse. N. Coronal streamers. Vrot=. 300 km/s. 200 km/s. 250 km/s. 350 km/s. 400 km/s. 450 km/s. WR wind bubble NGC 2359. Superbubble in the

174 views • 1 slides