The Latest Solar Images

Observations are happening daily, except for most Saturdays, all Sundays, and holiday periods; and are governed by duty schedule, weather, and solar activity. When the Sun has very low activity (spotless), observations will be limited or non-existent. Whenever the Sun becomes active again, the observing program will become active as well, weather permitting. The Sun is expected to reach the maximum activity level of the current Cycle 25 solar cycle. So we anticipate more events in terms of active region size and number, and solar flares.

One can monitor the Sun via several websites that provide real-time images of the Sun. The website, https://www.solarmonitor.org/, has such images in six different channels. The numbers are the NOAA designations for active regions (with the “1” at the start of the designation removed for convenience). Another website with up-t0-date information on solar activity and other goings-on in the skies is www.spaceweather.com. Additional information about the Sun’s current activity can be obtained from https://www.swpc.noaa.gov/, and real-time full-disk H-alpha images from observatories around the world can be viewed at http://halpha.nso.edu/.

A typical observing run may last from one to four hours, depending on seeing considerations, weather, and other work responsibilities, but will include active region monitoring of available active regions and the collection of frames for high-resolution solar mosaics in H-alpha. Each session includes at least one mosaic, which is a series of images made of all parts of the Sun’s disk that can later be stitched together to form a whole-disk image. At the very least, this ensures that all visible features such as prominences, filaments, and active regions (sunspot groups) are all captured in image form at least once per session. Usually observations are carried out in the late morning hours, but an additional session may occur in the mid-afternoon hours and it will include its own mosaic. If a sunspot group is expected to be active, then it becomes a main focus for observation for extended periods of time.

Solar activity is summarized in each day’s entry below, based on the forecast discussion product issued by the Space Weather Prediction Center each morning, along with observed activity (or lack of) the day of the featured observations. Regions are numbered by the NOAA/SWPC and are often provided in four-digit format (e.g. 3327), although I and other sources use the full five-digit designation (13327). Solar flares are described in terms of their X-ray intensity and optical “importance” (apparent brightness and area covered). One can learn more about the X-ray class of solar flares often discussed below by going to this website: https://www.spaceweather.com/glossary/flareclasses.html. Finally the SWPC 3-day forecast for solar activity is provided at the end of each entry.

More information about solar flares can be found at these websites: https://www.swpc.noaa.gov/phenomena; https://www.space.com/solar-flares-effects-classification-formation; and https://www.spaceweatherlive.com/en/solar-activity/solar-flares.html. I have also found the following website to be very useful: spaceweatherlive.com

The solar images are recorded through a Meade 16-inch f/8 Cassegrain telescope equipped with a 0.3 Å Hydrogen-alpha filter and a 16-bit, 3326×2504 pixel SBIG STF-8300 CCD camera. The aperture of the scope is stopped to 4-7/8 inch by an energy-rejection filter, which renders the system an f/26. A neutral density filter is added to bring the sunlight intensity down by 90%. Each image is automatically dark-subtracted as it is saved and each exposure is 0.1 second long for the red off-band continuum images and 0.5 second for the on-band H-alpha images. Flat field images are taken at periodic intervals throughout the observing session and are obtained by training the telescope to focus near the center of the Sun’s disk. Five images are then taken while dithering the frame 1′ to 5′ N,S,E, and W. The idea is to try to get images that are slightly blurred (either due to seeing or scope motion) and off set from each other. A set of 30 bias images (0-second exposures with the dome closed and scope parked) are taken at the end of each observing session.

Select images are processed for further study and display. A program called MaxIM DL is used to do basic calibration (bias-subtraction and flat field correction), and the levels are adjusted for optimum display contrast. Choice images are then selected for online display. All of the images are archived in their raw FITS format, sorted by date, and backed up twice. At a later time we can mass process these and make them available for scientific use. Inquiries can be made of Brian Cudnik, at bmcudnik@pvamu.edu, or Premkumar Saganti, at pbsaganti@pvamu.edu.]

NOTE: Images of the March 14, 2025 total lunar eclipse are posted at https://www.pvamu.edu/pvso/cosmic-corner/total-lunar-eclipse-1/

NOTE: Images of the April 8, 2024 solar eclipse are posted at https://www.pvamu.edu/pvso/cosmic-corner/partial-solar-eclipse/.

Observations have been conducted since then at the PVSO, primarily with H-alpha. There was a period of time when magnetospheric data were collected but the work had primarily been regional H-alpha images of active regions and filaments. Regular observations continued through the mid-2000’s, then became more sporadic through 2015. After a five-year pause, regular observations resumed (in their current format) on 8 January 2020.

January 19, 2026

Solar activity reached high levels yesterday (18 January) as a result of a long-duration X1.9/3B flare from AR 14341. This event peaked at 18:09 UT on 18 January. This launched a coronal mass ejection that took only 25 hours to impact the Earth’s magnetic field, producing widespread bright aurorae in Europe. There are eleven spotted active regions on the Sun.

After the X1.9 flare, solar activity returned to moderate levels, before trending to low later in the day. AR 14345 produced an M1.1 flare at 11:19 UT on 19 January. It the produced 8 C-class flares, ranging from C2 to C8 throughout the day. Only one other region flared, AR 14342, producing a C2. AR 14341 remained quiet all day long.

The first column below includes red continuum images, each 0.15 sec exposure; and the second column hosts H-alpha line center images, each 0.15 sec exposure. Each of the images covers 7.8’x11.4′ on the sky, unless indicated otherwise. Celestial north is up, west is right in each image.

More spotted groups are visible on the Sun these days.	This zone on the Sun was rather active, with most of the flare activity coming from the small spot group below AR 14341.
Two spot groups are visible on this part of the Sun.	AR 14347 (single spot, left), and 14342 (just right of center).
Some additional spots trail the main centers of activity and are labeled above.	This zone of the solar disk, remains quiet for the time being.

Solar activity is likely to be moderate, with a slight chance of additional X-class flares through 21 January.

January 16, 2026

Solar activity was low. The largest flare so far today (through 22:30 UT, 16 Jan.) was a C6.6/SF from AR 14345, a newly formed region just south of AR 14341. AR 14341 continues to be the largest (420 MSH) and most complex (beta-gamma-delta magnetic configuration) active region on the visible solar disk but it also remained quiet all day. It only produced two optical subflares and a C1 so far today.

The first column below includes red continuum images, each 0.09 sec exposure; and the second column hosts H-alpha line center images, each 0.15 sec exposure. Each of the images covers 7.8’x11.4′ on the sky, unless indicated otherwise. Celestial north is up, west is right in each image.

AR 14336 departs over the west limb. It is the second largest spot at 150 MSH	AR 14336 (and this zone of the Sun) has been completely quiet today. Two filaments remain visible north of the region.
AR 14343 lower part) and 14340 (upper right). AR 14343 continues to grow while 14340 continues to decay.	AR 14343 was the source of 2 C1 flares and one c4 flare today. This was one of the most active spot groups today.
AR 14342 (top center), 14347 (single spot near limb, upper left) and 14341 (bottom center).	These regions were relatively quiet today. A filament is visible toward the right of the image.

Solar activity is expected to be low, with a chance for M-class flares and a slight chance for X-class flares through 18 January.

January 15, 2026

Solar activity was at moderate levels due to an M1.6 flare that happened at 20:33 UTC on 14 January from AR 14341. This region also produced a C9.7 flare at 6:36 UTC on 15 January. Since then, and through 00:10 UTC, 16 January, solar activity returned to low levels, with only infrequent low-level C-class flaring. AR 14343 has grown quite a bit since yesterday, but was otherwise inactive. A Coronal Mass Ejection came from the area of AR 14340, but the bulk of this debris has been launched northward and is expected to miss the Earth.

The lone spot AR 14336 is rotating toward the limb of the Sun.	This image also includes a filament (top center), along with an inactive AR 14336.
AR 14340 (top center) and 14343 (below left), the latter of which has grown since yesterday.	This zone of the sun remains quiet, with 14340 nearly disappearing in H-alpha.
AR 14341 (below left), 14342 (upper right) and 14343 (lower right),	AR 14341 (lower left) and 14342 (upper left), along with a filament (just right of image center).

Solar activity is expected to be low, with a 25-30% chance for M-class flares from 15 to 17 January.

January 14, 2026

Solar activity is now back to moderate levels. The largest flare over the last 7 days was an M3.3 at 23:10 UTC on 11 July from AR 14341, which was behind the solar limb at the time. Then there was a C9.6 at 3:50 UTC on 14 January. Just happened was an M1.6/1F at 20:32 UT from AR 14341. Slight decay occurred in AR 14334 (barely visible as a single spot) and 14336 (a large spot with a few attendants trailing behind). AR 14340, which emerged several days ago, has also demonstrated some decay. AR 14341 and 14342 are situated along the eastern limb of the Sun and contributed almost all of the flaring activity over the last two days.

This active region sported many more spots a few days ago but has decayed to what is visible in this image.	AR 14336 along with a single filament (upper left quadrant of image). This part of the Sun has been quiet.
AR 14340 nearing the solar central meridian.	AR 14340 (top center) has been quiet. In the lower left corner, the bright spot marks another region emerging into view.
AR 14341 (bottom) and AR 14342 (top) are rotating into view. Small spots from a newly emerging sunspot group are visible in the lower right corner of the image.	AR 14341 and 14342 as they rotate into view, led by a filament (just right of image center). A new sunspot group is emerging (lower right corner).

Solar activity is expected to be low, with a 25% chance for M-class flares from 14 to 16 January.