Two C flares and two M flares were measured by GOES during the past 24 hours. A long duration M4.0 flare occurred in the western part of NOAA AR 11944 on January 4 with peak time at 19:46 UT. An associated CME is mainly propagating southward, but more properties are difficult to determine due to a data gap in STEREO and LASCO imagery. NOAA AR 11944 continued to grow in size and number of sunspots. It currently has a beta-gamma-delta magnetic configuration of its photospheric field. A long duration M2.0 flare erupted on January 4 with peak time at 22:52 UT. The source region for this event is NOAA AR 11936, currently located at the west limb. A related CME was observed in LASCO/C2 and STEREO B coronagraphic imagery (first measurement in LASCO/C2 at 23:12 UT). Based on the current observations, the CME is mainly propagating in the northwest direction with an estimated projected speed of 520 km/s. A glancing blow might arrive at Earth on January 8 around 0:00 UT. The >10 MeV proton flux was enhanced during the past 12 hours, but remained below the threshold level. The flaring chances for the next 48 hours are high: 90% for C flares, 70% for M flares. There is also some chance for an X flare (20%). We maintain the warning condition for proton events. Current solar wind speed measured by ACE is around 450 km/s. The magnitude of the interplanetary magnetic field remains around 4 to 6 nT. Current geomagnetic conditions are quiet (K=0 to 2) to unsettled (K=3) (estimated NOAA Kp 1 to 2 and K_Izmiran 1 to 3). Mainly quiet to unsettled conditions are expected to continue for the next 48 hours.
Equipment: Coronado 90 + SBIG 8300s + LX75
Time UT: 19:00
Exposure 0.8 sec.
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Image Credit & Copyright:
P.-A. Duc (CEA, CFHT), Atlas 3D Collaboration
What’s happening to galaxy NGC 474? The multiple layers of emission appear strangely complex and unexpected given the relatively featureless appearance of the elliptical galaxy in less deep images. The cause of the shells is currently unknown, but possibly tidal tails related to debris left over from absorbing numerous small galaxies in the past billion years. Alternatively the shells may be like ripples in a pond, where the ongoing collision with the spiral galaxy just above NGC 474 is causing density waves to ripple though the galactic giant. Regardless of the actual cause, the above image dramatically highlights the increasing consensus that at least some elliptical galaxies have formed in the recent past, and that the outer halos of most large galaxies are not really smooth but have complexities induced by frequent interactions with — and accretions of — smaller nearby galaxies. The halo of our own Milky Way Galaxy is one example of such unexpected complexity. NGC 474 spans about 250,000 light years and lies about 100 million light years distant toward the constellation of the Fish (Pisces).
NASA APOD 05-Jan-2014
The North America Nebula is large, covering an area of more than four times the size of the full moon; but its surface brightness is low, so normally it cannot be seen with the unaided eye. Binoculars and telescopes with large fields of view (approximately 3°) will show it as a foggy patch of light under sufficiently dark skies. However, using a UHC filter, which filters out some unwanted wavelengths of light, it can be seen without magnification under dark skies. Its prominent shape and especially its reddish color (from the hydrogen Hα emission line) show up only in photographs of the area.
Cygnus’s Wall is a term for the “Mexico and Central America part” of the North America Nebula. The Cygnus Wall exhibits the most concentrated star formations in the nebula.
Camera : SBIG STF-8300M (cooled at-5C)
Telescope/Lens : Takahashi FSQ-85ED (450mm f/5.3)
Filter : Astrodon Ha, SII, OIII
Tracking Mount : Takahashi EM-11
Autoguide : SBIG SG-4
Total Exposure Time : Ha-70mins, SII-60mins, OIII-55mins
w Dark Frames, Bias Frames
process w CCD stack,PI, PS5
Autor: Vincent Vegabort
AstroPhotography of the day by SPONLI
5 January 2014
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