Flaring activity increased slightly during the past 24 hours, with two C-class flares. A C1.1 flare erupted from Catania sunspot group 35 (NOAA AR 2050) and peaked at 1:26 UT on 30 April. Also a C1.5 flare was detected (peak at 6:20 UT on 30 April), and SDO imagery indicates Catania sunspot group 33 (NOAA AR 2047) as source. Catania sunspot group 33 produced a B9 flare peaking at 22:54 UT on 29 April. The B9 flare was accompanied by a coronal dimming, which indicates the occurrence of CME. A CME was observed in LASCO/C2 with first measurement at 00:24 UT on 30 April. Further analysis of this CME will be carried out, once more data are available. A filament eruption (centered at around E20N25) was visible in PROBA2/SWAP and SDO imagery, starting at 8:27 UT on 30 April. More C-class flares are possible during the next 48 hours. Solar wind observations of ACE indicated the arrival of a transient near 19:30 UT on 29 April. There is no clear signature of the arrival of the expected coronal hole high-speed stream.
Solar wind speed (near 300 km/s) is still low. The magnitude of the interplanetary magnetic field currently is around 10 nT, with a south-directed vertical component. This lead to a few time slots with unsettled geomagnetic conditions, which is expected to continue for the next few hours. Quiet geomagnetic conditions are expected from 1 May on.
Equipment: Coronado 90 + Imaging Source DMK + LX75
Processing: Photoshop, Avistack 300 frames
Time UT: 15:00
Exposure 1/500 sec.
With SPONLI Space is getting closer
Image Credit & Copyright: Andrew Wall
If you look closely, you will see something quite unusual about this setting Sun. There are birds flying to the Sun’s left, but that’s not so unusual. A dark sea covers the Sun’s bottom, and dark clouds cover parts of the middle, but they are also not very unusual. More unusual is the occulted piece at the top right. And that’s no occulting cloud — that’s the Moon. Yesterday the Moon moved in front of part of the Sun as visible from Australia, and although many locations reported annoying clouds, a partially eclipsed Sun would occasionally peak through as it set. The above image was captured yesterday on the western horizon of Adelaide, South Australia. The maximum eclipse was visible only from a small part of Antarctica where the entire Moon could be seen covering the entire center of the Sun in what is known as an annular eclipse, leaving only a ring of firefrom the Sun peaking out around the edges. The next solar eclipse will be another partial eclipse, will occur on 2014 October 23, and will be visible from most of North America near sunset.
NASA APOD 30-Apr-14
NGC 2174 (also known as Monkey Head Nebula) is an H II emission nebula located in the constellation Orion and is associated with the open star cluster NGC 2175. It is thought to be located about 6,400 light-years away from Earth. The nebula may have formed through hierarchical collapse.
There is some equivocation in the use of the identifiers NGC 2174 and NGC 2175. These may apply to the entire nebula, to its brightest knot, or to the star cluster it includes. Burnham’s Celestial Handbook lists the entire nebula as 2174/2175 and does not mention the star cluster. The NGC Project (working from the original descriptive notes) assigns NGC 2174 to the prominent knot at J2000 06h 09m 23.7s, +20° 39′ 34″ and NGC 2175 to the entire nebula, and by extension to the star cluster. Simbad uses NGC 2174 for the nebula and NGC 2175 for the star cluster.
Imaging telescopes or lenses: Williams Optics Megrez 72
Imaging cameras: Starlight Xpress SXVR-H9
Mounts: Sky-Watcher HEQ5 PRO
Guiding telescopes or lenses: Williams Optics Megrez 72
Guiding cameras: Starlight Xpress CoStar
Focal reducers: William Optics FF/FR VI
Software: PixInsight 1.8, PHD guiding, Nebulosity 3, EQMac
Filters: Astrodon 3nm OIII, Astrodon Ha 5nm
Accessories: Starlight Xpress Mini Filter wheel
Dates: Jan. 25, 2014, Jan. 26, 2014
Astrodon 3nm OIII: 10×1800″ -20C
Astrodon Ha 5nm: 10×1800″ -20C
Integration: 10.0 hours
AstroPhotography of the day by SPONLI
30 April 2014
Пять групп солнечных пятен зарегистрированы на видимой стороне солнечного диска. Группа солнечных пятен 2049 показала некоторый рост. Остальные группы были стабильными. Одна вспышка C3.4 вспышка с пиком в 15:26 UT 28 апреля произошла в регионе 2048.
Возможно образование новых вспышек С-класса в течение следующих 48 часов. Не обнаружены направленные на землю выбросы корональной массы. Скорость солнечного ветра снизилась до только 280 км/с. Величина межпланетного магнитного поля в настоящее время ниже 5 нТл. Геомагнитные условия были тихими и, как ожидается, останутся таковыми. Все еще возможны интервальные возмущения магнитосферы, в связи с вероятным прибытием высокоскоростного потока от корональной дыры, которые пересекла центральный меридиан утром 24 апреля.
Оборудование: Coronado 90 + LX75 + Imaging Source DMK
Обработка: PS, Avistack 300
Время по МСК: 20:00
Выдержка 1/150 сек.