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Щоденний бюлетень про сонячну та геомагнітну активність від SIDC

Випущено: 2026 May 31 1231 UTC

Прогноз SIDC

Сонячні спалахи

C-class flares expected, (probability >=50%)

Геомагнетизм

Quiet (A<20 and K<4)

Сонячні протони

Quiet

	10 см потік	Ap
31 May 2026	140	008
01 Jun 2026	138	010
02 Jun 2026	136	010

Сонячно-активні області та спалахи

Solar flaring activity has been low over the last 24 hours, with a few C-class flares. The strongest flare was a C3.1 flare (SIDC Flare 7810) peaking at 02:09 UTC on May 31, associated with SIDC Sunspot Group 873 (NOAA Active Region 4446, magnetic type beta). There are currently nine numbered active regions on the solar disk. The most complex ones have a beta magnetic type. SIDC Sunspot Groups 805, 862, 874 and 876 (NOAA Active Regions 4445, 4443, 4448 and 4451) have decayed into plage. The solar flaring activity is expected to be low over the next 24 hours, with C-class flares very likely and a small chance for M-class flares.

Корональні викиди маси

A narrow Coronal Mass Ejection (SIDC CME 663) was observed in LASCO/C2 and STEREO-A coronagraph imagery, lifting off from the northeast limb, starting from 07:30 UTC on May 31. It is associated with a prominence eruption observed in AIA 304 data around 05:00 UTC on May 31 over the northeast limb. It is not expected to impact Earth. No other Earth-directed CMEs were observed in the available coronagraph imagery during the last 24 hours.

Корональні діри

An equatorial, positive polarity coronal hole (SIDC Coronal Hole 166) is crossing the central meridian. An associated high-speed stream may arrive at Earth starting from the UTC morning on June 03.

Сонячний вітер

Over the last 24 hours, the solar wind parameters (ACE and DSCOVR) were enhanced, likely due to the ongoing influence of high-speed streams from the two negative polarity coronal holes (the northern SIDC Coronal Hole 142 and the equatorial SIDC Coronal Hole 165, which crossed the central meridian on May 27 and May 28 respectively). The solar wind speed increased from 400 km/s to 560 km/s. The interplanetary magnetic field decreased from 11 nT to around 5 nT. The Bz component varied between -10 nT and 5 nT. The interplanetary magnetic field angle phi was predominantly in the negative sector. Over the next 24 hours, enhanced solar wind conditions may still be observed initially, followed by a gradual return to the slow solar wind regime.

Геомагнетизм

Geomagnetic conditions globally were initially quiet (NOAA Kp 2) and then reached active levels (NOAA Kp 3- to 4+ ) between 18:00 UTC on May 30 and 03:00 UTC on May 31. Geomagnetic conditions locally were initially quiet to unsettled (K Bel 2 to 3), reaching active levels between 18:00 UTC and 22:00 UTC on May 30. Mostly quiet conditions, with possible isolated intervals of unsettled or active conditions, are expected over the next 24 hours.

Рівні потоку протонів

The greater than 10 MeV proton flux was below the 10 pfu threshold during the last 24 hours. It is expected to remain below the threshold level over the next 24 hours.

Потоки електронів на геостаціонарній орбіті

The greater than 2 MeV electron flux measured by GOES 18 and GOES 19 was elevated but remained below the 1000 pfu threshold during the last 24 hours. The 24-hour electron fluence was at normal levels and it is expected to remain so over the next 24 hours.

Розрахунок міжнародної кількості сонячних плям станом на сьогодні (ISN): 120, за даними 12 станцій.

Сонячні індекси за 30 May 2026

Число Вольфа, Катанія	///
Сонячний потік 10 см	142
AK Chambon La Forêt	030
AK Wingst	016
Розрахунковий індекс Ap	017
Розрахункова міжнародна кількість сонячних плям	133 - За даними 27 станцій

Зведення помітних подій

Надано Центром Аналізу Даних Сонячного Впливу (SIDC)© - SIDC - Оброблено SpaceWeatherLive

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