Heliophysics Science: -Energy of Solar Flares

Heliophysics Science:
High‑Energy Aspects of Solar Flares

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Organization National Aeronautics and Space Administration (NASA)

Reference Code 0032‑NPP‑MAR
26‑GSFC‑Helio Sci

How to Apply All applications must be submitted in Zintellect. Please visit the NASA Postdoctoral Program website for application instructions and requirements.

Final date to receive applications 3/1/2026 6:00:59 PM Eastern Time Zone

Description The acceleration of charged particles to high energies and their confinement, transport, and subsequent energy losses are among the fundamental processes of solar flares. We investigate these processes through observations of X‑rays and gamma rays and through theoretical modeling.

Our most recent observational effort was the Reuven Ramaty High‑Energy Solar Spectroscopic Imager (RHESSI), a Small Explorer mission operational from February 2002 through April 2018. It conducted the first high‑resolution X‑ray and gamma‑ray imaging spectroscopy of solar flares using cooled germanium detectors and Fourier‑transform imaging in the energy range from 3 keV to 20 MeV. RHESSI obtained a wealth of observations that are reshaping our understanding of particle acceleration in flares.

We also analyze data sets from X‑ray and gamma‑ray instruments on the Solar Maximum Mission, the Compton Gamma Ray Observatory, the Japanese Yohkoh spacecraft, and the Fermi astrophysics mission. Complementary observations from ground‑based radio and optical instruments are also available. This comprehensive array of observational data is available online at the Solar Data Analysis Center in Goddard’s Solar Physics Branch, and its detailed analysis is providing critical tests of theoretical models of solar flares.

We are developing an integrated package of modular numeric codes and models for the analysis and interpretation of these data. The package focuses on energetic electrons produced during the impulsive phase of flares, computing bremsstrahlung X‑ray/gamma‑ray emission and gyrosynchrotron radio emission from model flare configurations. Steady‑state and time‑dependent Fokker‑Planck codes compute transport of suprathermal electrons. A hydrodynamic code will compute the response of the flare plasma.

The package will allow comprehensive modeling of energized electrons in different flare scenarios, and the predicted emissions can be compared directly with X‑ray/gamma‑ray and radio images and spectra.

We also have research programs to develop solid‑state detectors with high spectral resolution, high‑spatial resolution scintillation detectors for hard X‑ray imaging, and a new telescope concept using high‑Z Fresnel Zone Plates to image at hard X‑ray energies.

Solar physics background is an advantage but is not required.

Location Goddard Space Flight Center, Greenbelt, Maryland

Field of Science Heliophysics Science

Advisors
Steven Christe – steven.d.christe – 301‑286‑7999
Albert Y. Shih – albert.y.shih – 301‑286‑1843

Applications with citizens from Designated Countries will not be accepted at this time, unless they are Legal Permanent Residents of the United States.

Eligibility is currently open to:

• U.S. Citizens;
• U.S. Lawful Permanent Residents (LPR);
• Foreign Nationals eligible for an Exchange Visitor J‑1 visa status;
• Applicants for LPR, asylees, or refugees in the U.S. at the time of application with a valid EAD card and I‑485 or I‑589 forms in pending status.

Eligibility Requirements

• Degree:
  Doctoral Degree.

Questions about this opportunity? Please email or contact the point of contact, Mikeala.