The Sun giving out a large geomagnetic storm on 1:29 pm, EST, 13th March 2012
Hey Everybody!!!! Come On In-
I found some new views from the old Sun!! And a great Feature Presentation Video for our viewing pleasure tonight.
Welcome to the new people coming in for the first time! This Nature Blog is a collection of posts generally regarding the Nature of Mother Earth, Father Space or Human Nature! Each post is a different subject, so if you do not care for one, try another from the selection on the right. You can also subscribe by email if you want notification of the posts (or friend connect Google Reader).
We are enjoying a world tour through You Tube Videos. I gather information from the internet pertinent to each subject, however, learning is completely optional. It is my hope that my Grandchildren will come to the Blog when they are old enough to read!
Tonight our journey takes us to the Sun. I thought it would be nice to Light Up Your Life!!! Enjoy your photostudy.
Photo Gallery: Sun
Glowing Sun
Photograph courtesy NASA
An enormous magnetic loop of hot gases creates a glowing handle on the sun. The June 9, 2002, prominence was caused by explosive instabilities in the sun's magnetic field.
Coronal Loops
Photograph courtesy NASA
Magnetism made visible: That describes virtually every feature on the sun, from sunspots to these soaring structures, called loops. Loops easily reach the height of ten Earths. Energy generated by the dynamics of smaller loops is likely the source of the solar corona's mysterious heat. The superheated gases that form the sun, mainly hydrogen and helium, exist in an electrified state called plasma. Below the surface, plasma can push and drag magnetic field lines. But when lines are strong enough to arc out, wildly conductive plasma follows.
Sunspot Loops
Photograph courtesy NASA
It may look wild, but this image of the solar surface, captured by a NASA satellite called TRACE in 2000, was described by scientists as "a quiet day on the sun." In other words, spectacular loops but no storms.
Sun Storm
Photograph courtesy NASA/JPL
The sun-orbiting SOHO spacecraft captured this snapshot of the development of a coronal mass ejection (CME), an explosive sun storm. It shows erupting filaments lifting off the active solar surface and blasting enormous bubbles of magnetic plasma into space. CMEs occur anywhere from once a week to two or more times a day, and they can profoundly influence space weather.
Composite Sun
Photograph courtesy NASA/ESA
This SOHO image is in extreme-ultraviolet wavelengths, color-coded by temperature, with red showing the hottest. Why is the halo-like corona, visible from Earth only during a total eclipse, hundreds—even thousands—of times hotter than the sun's surface? That's one of the questions that keep scientists looking straight at the sun.
Just Push Play
 | |
| Observation data | |
|---|---|
| Mean distance from Earth | 1.496×108 km 8 min 19 s at light speed |
| Visual brightness (V) | −26.74 [1] |
| Absolute magnitude | 4.83 [1] |
| Spectral classification | G2V |
| Metallicity | Z = 0.0122[2] |
| Angular size | 31.6′ – 32.7′ [3] |
| Adjectives | Solar |
| Orbital characteristics | |
| Mean distance from Milky Waycore | ~2.5×1017 km 26,000 light-years |
| Galactic period | (2.25–2.50)×108 a |
| Velocity | ~220 km/s (orbit around the center of the Galaxy) ~20 km/s (relative to average velocity of other stars in stellar neighborhood) ~370 km/s[4] (relative to the cosmic microwave background) |
| Physical characteristics | |
| Mean diameter | 1.392×106 km [1] 109 × Earth |
| Equatorialradius | 6.955×105 km [5] 109 × Earth[5] |
| Equatorialcircumference | 4.379×106 km [5] 109 × Earth[5] |
| Flattening | 9×10−6 |
| Surface area | 6.0877×1012 km2 [5] 11,990 × Earth[5] |
| Volume | 1.412×1018 km3 [5] 1,300,000 × Earth |
| Mass | 1.9891×1030 kg[1] 333,000 × Earth[1] |
| Average density | 1.408×103 kg/m3 [1][5][6] |
| Density | Center (model): 1.622×105 kg/m3 [1] Lower photosphere: 2×10−4 kg/m3 Lower chromosphere: 5×10−6 kg/m3 Corona (avg): 1×10−12 kg/m3 [7] |
| Equatorialsurface gravity | 274.0 m/s2 [1] 27.94 g 28 × Earth[5] |
| Escape velocity (from the surface) | 617.7 km/s [5] 55 × Earth[5] |
| Temperature | Center (modeled): ~1.57×107 K [1] Photosphere (effective): 5,778 K [1] Corona: ~5×106 K |
| Luminosity(Lsol) | 3.846×1026 W [1] ~3.75×1028 lm ~98 lm/W efficacy |
| Meanintensity (Isol) | 2.009×107 W·m−2·sr−1 |
| Age | 4.57 billion years[8] |
| Rotation characteristics | |
| Obliquity | 7.25° [1] (to the ecliptic) 67.23° (to the galactic plane) |
| Right ascension of North pole[9] | 286.13° 19 h 4 min 30 s |
| Declination of North pole | +63.87° 63° 52' North |
| Sidereal rotation period (at equator) | 25.05 days [1] |
| (at 16° latitude) | 25.38 days [1] 25 d 9 h 7 min 12 s [9] |
| (at poles) | 34.4 days [1] |
| Rotation velocity (at equator) | 7.189×103 km/h [5] |
| Photospheric composition (by mass) | |
| Hydrogen | 73.46%[10] |
| Helium | 24.85% |
| Oxygen | 0.77% |
| Carbon | 0.29% |
| Iron | 0.16% |
| Neon | 0.12% |
| Nitrogen | 0.09% |
| Silicon | 0.07% |
| Magnesium | 0.05% |
| Sulfur | 0.04% |
The Sun, from my perspective:
**************************************
Feature Presentation: The Most Interesting Sun Vid Yet!! Just Push Play
http://en.wikipedia.org/wiki/Sun
1. Core
2. Radiative zone
3. Convective zone
4. Photosphere
5. Chromosphere
6. Corona
7. Sunspot
8. Granules
9. Prominence.
Just Push Play
...this is brendasue signing off from Rainbow Creek
See You Next Time. Love Ya!
http://en.wikipedia.org/wiki/Sun
http://en.wikipedia.org/wiki/File:Sunspots_and_Solar_Flares.jpg
The Sun giving out a large geomagnetic storm on 1:29 pm, EST, 13th March 2012
Of course, one more Great Performance, Push Play
image credits:
Photo Gallery: Sun
http://science.nationalgeographic.com/science/photos/sun-gallery/#/glowing-sun-prominence_6594_600x450.jpg
O+O
