Daily Archives: January 21, 2014

The Sun Online and solar activity. January 21, 2014

Ten sunspot groups were reported by Catania today. The Catania sunspot group 17 (NOAA AR 1959) developed the beta-gamma configuration of its photospheric magnetic field and produced four C-class flares yesterday. The strongest flare of the past 24 hours was the C3.6 flare peaking at 22:49 UT
on January 20 in the Catania sunspot group 20 (no NOAA number yet). We expect flaring activity on the C-level from these two groups, with an M-class flare possible but not very likely.
The above-mentioned C3.6 flare was accompanied by a halo CME first visible in the SOHO/LASCO C2
field of view at 22:12 UT. The bulk of the CME erupted toward the east, but there were weak extensions to form a full halo. The projected plane-of-the-sky speed of the CME was around 1000 km/s (with a big
uncertainty due to a not well-formed front). SDO/AIA data show that the CME was associated with coronal dimmings and a post-eruption arcade. Only the CME-driven shock may arrive at the Earth on January 24, although it is unlikely. In case of the shock arrival, the geomagnetic conditions are not
expected to go above active (K = 4). Another halo CME (this time a partial one) was first observed in the SOHO/LASCO C2 field of view at 15:24 UT on January 20. The CME had the angular width of around 230 degrees and the speed around 550 km/s. STEREO/EUVI B data show that the CME was associated with a far side eruption (as seen from the Earth) with the source region located around S15E170. This CME will therefore not arrive at the Earth and have no geomagnetic consequences. The interplanetary
magnetic field (IMF) magnitude reached 10 nT in the past hours, indicating the arrival of the interaction region between the slow and the fast solar wind flows. The IMF Bz component is increased but fluctuating between positive and negative values. Currently the solar wind speed is still low (between 300 and 350 km/s), but the arrival of the fast flow from the low-latitude coronal hole in the northern hemisphere is still expected today. Active geomagnetic conditions will be possible.

Equipment: Coronado 90 + SBIG 8300s + LX75
Processing: Photoshop
Date: 01/21/14
Time UT: 19:00
Exposure 0.8 sec.

With SPONLI Space is getting closer!


Micro Moon over Super Moon

Image Credit: Stefano Sciarpetti
Explanation: Did you see the big, bright, beautiful Full Moon last Wednesday night? That was actually a Micro Moon! On that night, the smallest Full Moon of 2014 reached its full phase only a few hours from lunarapogee, the time of its the most distant point from Earth in the Moon’s elliptical orbit. Of course, last year on the night of June 22, a Full Super Moon was near perigee, the closest point in its orbit. The relative apparent sizeof January 15’s Micro Moon is compared to the June 22 Super Moon in the above composite image digitally superimposing telescopic images from Perugia, Italy. The difference in apparent size represents a difference in distance of just under 50,000 kilometers between apogee and perigee, given the Moon’s average distance of about 385,000 kilometers. How long do you have to wait to see another Full Micro Moon? Until March 5, 2015, when the lunar full phase will again occur within a few hours of lunar apogee.

NASA APOD 21-Jan-2014

The Pelican Nebula

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The Pelican Nebula (also known as IC 5070 and IC 5067) is an H II region associated with the North America Nebula in the constellation Cygnus. The gaseous contortions of this emission nebula bear a resemblance to a pelican, giving rise to its name. The Pelican Nebula is located nearby firstmagnitude star Deneb, and is divided from its more prominent neighbour, the North America Nebula, by a molecular cloud filled with dark dust.

The Pelican is much studied because it has a particularly active mix of star formation and evolving gas clouds. The light from young energetic stars is slowly transforming cold gas to hot and causing an ionization front gradually to advance outward. Particularly dense filaments of cold gas are seen to still remain, and among these are found two jets emitted from the Herbig–Haro object 555. Millions of years from now this nebula might no longer be known as the Pelican, as the balance and placement of stars and gas will leave something that appears completely different.

Imaging telescopes or lenses: Teleskop Service 10″ Newton F4.8
Imaging cameras: Atik 383L+
Mounts: Astro-Physics Mach 1 GTO
Guiding telescopes or lenses: Teleskop Service 10″ Newton F4.8
Guiding cameras: Orion StarShoot Autoguider
Focal reducers: ASA 2″ x 0,73 Corrector/Reducer 2KORRR
Software: PixInsight PixInsinght 1.8 RC7
Filters: Baader Planetarium Baader 2″ Narrowband Set
Dates: Sept. 4, 2013
Frames: Baader Planetarium Baader 2″ Narrowband Set: 14×400″ -20C bin 1×1
Integration: 1.6 hours
Darks: ~20
Flats: ~20
Flat darks: ~20
Bias: ~20

Autor: Pekka Simell

AstroPhotography of the day by SPONLI

21 January 2014

We select the best works of amateur astrophotographers with details of equipment, shooting processing etc.