V7993 Sgr finder map
V7993 Sgr finder map
We have a new "star" in the night sky. In truth, it's been there for billions of years, but only first revealed itself a little more than a week ago. Nova Sagittarii 2025 No. 3 was independently discovered on March 23-24 by the Russian New Milky Way (NMW) Survey and Japanese amateur Tadashi Kojima at right ascension (R.A) 18h 02′, declination (Dec) –33° 11′. Both parties caught the star around magnitude 13; two days later it had risen to 10.5. Despite it southerly declination the nova stands more than 10° above the horizon before the start of dawn, making it an attainable target even for observers in the northern U.S.
V7993 Sgr AAVSO map
V7993 Sgr AAVSO map
Clouds have thwarted my attempts to see it, but the most estimate posted to the AAVSO peg it at magnitude 10.7 on April 1st. Not long after discovery, the star received its official designation V7993 Sagittarii, making it the 7,993 variable star to be discovered in Sagittarius. Although novae can appear anywhere in the sky, they're far more common within the star-dense band of the Milky Way and especially in Sagittarius, where we face toward the galactic center. In fact, this is the third nova discovered so far this year in the constellation.
This animation depicts an outburst of the recurrent nova T CrB but also demonstrates the nova eruption process. Watch until the end for the exciting conclusion.
NASA's Goddard Space Flight Center Conceptual Image Lab
In last week's post, I described novae, recurrent novae and dwarf novae. All three types occur in close binary star systems, where one member is a hot, dense white dwarf and the other a normal star. In each case, material flows from the companion into a flattened cloud of hot gas spinning around the dwarf called an accretion disk. In a nova, material funnels down from the disk to the star's surface until sufficient mass has accumulated for heat and pressure to "ignite" the gas in a runaway thermonuclear explosion. The blast creates a brilliant fireball which slowly cools and fades. A recent measurement clocked V7993's expanding debris cloud at 700 kilometers a second (1.6 million mph). Despite the blast, the white dwarf remains intact after the blast and the process begins anew.
Novae generally skyrocket in brightness quickly then gradually fade over the weeks and months. Watching a nova dim (and occasionally re-brighten!) makes them great, long-term observing subjects. Use the AAVSO map and comparison stars to help you follow V7993 Sgr's variations.
Demon Star in eclipse
Algol-type eclipsing binary animation
Algol-type eclipsing binary animation
As a budding 11-year-old amateur astronomer, Algol in Perseus was my first variable star. I still remind myself to gaze its direction every clear night I'm out from fall through spring. Every 2.9 days the more massive but fainter star in this binary system eclipses the smaller, brighter companion. In full eclipse at minimum light, Algol shines weakly at magnitude 3.4 compared to its usual 2.1. The difference is very apparent with the naked eye.
If you've read about Algol and have never observed it (or it's been a while), you'll have the opportunity to see it in eclipse on the night of April 3rd. At 10:11 p.m. EDT that evening, the star will dim to minimum light. For one hour on either side of minimum, it remains near that brightness. But if you check 2 hours or more after minimum, you'll see it begin to recover in brightness.
Algol finder map
Algol finder map
Despite eclipses occurring at short intervals, they're visible only infrequently for any particular location. After the April 3rd event, the next widely and easily visible eclipse takes place on April 26th. For more eclipse times and additional information, visit Sky & Telescope's Minima of Algol calculator.
One night, two moons, three events
Jupiter has already begun its western descent. When a planet reaches a high declination it seems to stick around forever. Even taken for granted. But the writing's on the wall — the gas giant's good nights are dwindling. It's time for another look.
On the night of April 5-6, three separate events involving two Jovian moons occur in succession. First, observers in the eastern half of the U.S. and Canada will see Europa cast its tiny, black shadow on Jupiter's cloud tops from 6:16-8:54 p.m. CDT. While the first part of the shadow transit won't be visible due to Sun and / or twilight interference, we'll see Europa's shadow skirting the south edge of the Southern Equatorial Belt (SEB) in a darkening sky.
Jupiter moon phenomena
Jupiter moon phenomena
Starting at 9:22 p.m. CDT, Ganymede will emerge from occultation at the planet's northeastern limb, looking like a tiny pearl. A little more than two hours later, at 11:30 p.m., the same moon will slowly fade from sight as it enters Jupiter's shadow in eclipse. It won't poke back into the sunlight again until 2:04 a.m. To find out times of other watch-worthy Jovian moon events, visit Sky & Telescope's Jupiter's Moons site.
Uranus occults 9th magnitude star
Uranus occults HIP 16271
Uranus occults HIP 16271
On the evening of April 7th, Uranus will occult the 9.1 magnitude star HIP 16271 around 9:30 p.m. CDT (2:30 UT). Observers in central North America will have the best view. Farther east the planet will be too close to the horizon or have set, while in the western U.S., the occultation takes place in a bright sky. Even from the best locations it will still be challenging because the planet will be only about 15° high at the time.
Serious amateurs will attempt to record dips in the star's light as it's occulted by the planet's spindly rings prior to and after its disappearance behind the planet. More casual observers can watch Uranus slowly encroach on the star until the two merge into one. For full details, including a list of cities and times, check out occultation expert David Dunham's Uranus Occultation page.