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- 20:04, 19 October 2026 ALEXIS: When and Where is that Flare (hist | edit) [6,216 bytes] Hhudson (talk | contribs) (Created page with "{{Infobox Nugget |name = Nugget |title = Alexis: When and Where is that Flare? |number = 538 |first_author = Jorge R. PADIAL DOBLE |second_author = Kelly HOLLEY-BOCKELMANN |publish_date = October 26, 2026 |next_nugget = |previous_nugget = {{#ask: Category:Nugget RHESSI Nugget Index::537}} }} == A light curve without a location == Every X5.0 solar flare headline you have read about is named after a single number: the soft X-ray flux of the entire unresolved...")
- 11:10, 19 October 2026 Alexis: When and Where is that Flare? (hist | edit) [6,214 bytes] Hhudson (talk | contribs) (Created page with "{{Infobox Nugget |name = Nugget |title = Alexis: When and Where is that Flare? |number = 538 |first_author = Jorge R. PADIAL DOBLE |second_author = Kelly HOLLEY-BOCKELMANN |publish_date = October 26, 2026 |next_nugget = |previous_nugget = {{#ask: Category:Nugget RHESSI Nugget Index::537}} }} == A light curve without a location == Every X5.0 solar flare headline you have read about is named after a single number: the soft X-ray flux of the entire unresolved...")
- 19:39, 9 October 2026 The Hale Sector Boundary links flares to global magnetic fields (hist | edit) [4,014 bytes] Hhudson (talk | contribs) (No. 537 initial upload)
- 09:56, 27 September 2026 Photospheric flows in Sun-as-a-star EUV Doppler spectra (hist | edit) [6,349 bytes] Hhudson (talk | contribs) (No. 536 without figures)
- 16:24, 16 September 2026 Why do only some fast CMEs produce sustained gamma-ray emissions? (hist | edit) [4,871 bytes] Hhudson (talk | contribs) (Created page with "{{Infobox Nugget |name = Nugget |title = Why do only some fast CMEs produce sustained gamma-ray emissions? |number = 535 |first_author = Ratul MOHAN |publish_date = September 14, 2026 |next_nugget = |previous_nugget = {{#ask: Category:Nugget RHESSI Nugget Index::534}} }} == Introduction == Certain strong solar flares may accelerate particles producing intense gamma-ray emissions during their impulsive phase. In some flares, however, gamma rays with energies >...")
- 07:43, 4 September 2026 A New Route to Coronal Vector Magnetometry (hist | edit) [5,572 bytes] Hhudson (talk | contribs) (No. 534 initial upload)
- 14:57, 3 September 2026 Trading Stokes V for Wave Speeds: A New Route to Vector Coronal Magnetometry (hist | edit) [5,015 bytes] Hhudson (talk | contribs) (Created page with "{{Infobox Nugget |name = Nugget |title = Trading Stokes V for Wave Speeds: A New Route to Vector Coronal Magnetometry |first_author = Alin PARASCHIV |publish_date = September 1, 2026 |next_nugget = |previous_nugget = {{#ask: Category:Nugget RHESSI Nugget Index::533}} }} == Introduction == The magnetic field of the solar corona remains observationally elusive. At the same time, it is absolutely the most fundamental property defining all coronal activity. One o...")
- 19:31, 21 August 2026 The Variance of Solar X-ray Flux (hist | edit) [3,975 bytes] Hhudson (talk | contribs) (No. 533 initial upload)
- 08:11, 5 August 2026 Electron-Ion equilibration in CME-driven shocks (hist | edit) [5,516 bytes] Hhudson (talk | contribs) (No. 532 initial upload)
- 16:52, 3 August 2026 The Source Surface Height Through the Solar Cycle: A Path to Better Solar Wind Forecasts (hist | edit) [5,881 bytes] Hhudson (talk | contribs) (No. 531 initial upload)