{
  "abstract": "Context . A challenging issue is the significant velocity discrepancy between jets and energetic electrons accelerated by magnetic reconnection in solar flares.\n\nAims . We investigated the velocities of jets derived from extreme-ultraviolet (EUV) observations and those of energetic electrons inferred from type III radio bursts in two solar flares on 26 March 2024.\n\nMethods . The jet velocities were measured from the time-distance maps of the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA), while the energetic electron velocities were inferred from the type III radio burst spectra using the Aschwanden density model.\n\nResults . These two flares are homologous events occurring in the same active region of NOAA 13615. They produce jets and type III radio bursts detected by SDO/AIA, Daocheng Radio Telescope (DART), Chashan Broadband Solar Radio Spectrometer at meter wavelengths (CBSm), and Radio and Plasma Waves (RPW). Linear fits to the jet trajectories in the plane-of-sky yield jet velocities of 436 km s ⁻¹ and 456 km s ⁻¹ for the first and second flares, respectively. The corresponding type III electron beam velocities, inferred from the Aschwanden model fitting the CBSm data, are 32.3 Mm s ⁻¹ (or 0.1 c) and 22.0 Mm s ⁻¹ (or 0.07 c), respectively. These velocities correspond to the kinetic energies of 3.0 keV and 1.4 keV, which are much lower than the cutoff energies (i.e., 18 keV) detected by the Spectrometer/Telescope for Imaging X-rays (STIX). Moreover, our DART observations show type III burst sources as funnel-like structures varying in either frequency or height in both flares. Their sizes increase rapidly with decreasing frequency, such as a ninefold expansion from 477 MHz to 164 MHz, indicating the magnetic field decreases by a factor of nine from 0.04 R ⊙ (447 MHz) to 0.10 R ⊙ (164 MHz).\n\nConclusions . Jets are accelerated by magnetic pressure gradients, with inferred magnetic field strengths of about 60 G at the boundaries of the reconnection regions in both events. Type III electron beams are accelerated by electric fields, with strengths of 4.3–15 ×10 ⁻⁴ V m ⁻¹ and 1.0–3.7×10 ⁻⁴ V m ⁻¹ estimated in the current sheet for the first and second flares, respectively.",
  "abstract_shown": true,
  "affiliations": [
    "Key Laboratory of Dark Matter and Space Science, Purple Mountain Observatory, Chinese Academy of Sciences",
    "School of Astronomy and Space Science, University of Science and Technology of China",
    "School of Computer Science, Software Engineering and Cyberspace Security, Nanjing University of Posts and Telecommunications",
    "State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences"
  ],
  "article_type": null,
  "arxiv": null,
  "author_total": 11,
  "authors": [
    {
      "affs": [
        0,
        1
      ],
      "name": "Xiaoyu Tang",
      "orcid": "0009-0002-8761-0217"
    },
    {
      "affs": [
        0
      ],
      "name": "Zongjun Ning",
      "orcid": "0000-0002-9893-4711"
    },
    {
      "affs": [
        0,
        1
      ],
      "name": "Yuzhi Yang",
      "orcid": "0009-0005-5397-3329"
    },
    {
      "affs": [
        0,
        2
      ],
      "name": "Guotianci Xu",
      "orcid": "0009-0005-5306-3456"
    },
    {
      "affs": [
        0,
        1
      ],
      "name": "Yijie Han",
      "orcid": "0009-0001-7759-9504"
    },
    {
      "affs": [
        0,
        1
      ],
      "name": "Kangyi Li",
      "orcid": "0009-0008-1395-7430"
    },
    {
      "affs": [
        0
      ],
      "name": "Yu Huang",
      "orcid": "0000-0002-0937-7221"
    },
    {
      "affs": [
        3
      ],
      "name": "Jingye Yan",
      "orcid": "0000-0002-7597-7663"
    },
    {
      "affs": [
        3
      ],
      "name": "Li Deng",
      "orcid": "0009-0003-2125-5141"
    },
    {
      "affs": [
        3
      ],
      "name": "Lin Wu",
      "orcid": "0009-0009-6131-3581"
    },
    {
      "affs": [
        3
      ],
      "name": "Yujie Liu",
      "orcid": "0009-0003-0078-2057"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/5wbw6sr4ppzaz.bib",
  "cited_by": 0,
  "doi": "10.1051/0004-6361/202660823",
  "fulltext_url": null,
  "id": "5wbw6sr4ppzaz",
  "issns": [
    "0004-6361",
    "1432-0746"
  ],
  "landing_url": "https://www.aanda.org/10.1051/0004-6361/202660823",
  "language": null,
  "licence": "CC-BY-4.0",
  "licence_label": "CC BY 4.0",
  "licence_source": "article",
  "licence_url": "https://creativecommons.org/licenses/by/4.0",
  "metadata_licence": null,
  "native_subjects": [
    [
      "openalex",
      "3103|Solar and Space Plasma Dynamics"
    ]
  ],
  "openalex": "W7221708303",
  "pdf_url": null,
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-13",
  "publisher": "EDP Sciences",
  "ris": "https://research.draconitic.com/paper/5wbw6sr4ppzaz.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:18:18Z",
      "native_id": "10.1051/0004-6361/202660823",
      "source": "crossref",
      "url": "https://www.aanda.org/10.1051/0004-6361/202660823"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "openalex:3103|Solar and Space Plasma Dynamics",
      "subfield": "stellar"
    }
  ],
  "title": "Type III radio bursts associated with jets in two solar flares",
  "title_text": "Type III radio bursts associated with jets in two solar flares",
  "type": "peer-reviewed",
  "updated_at": "2026-10-30T12:18:18Z",
  "url": "https://research.draconitic.com/paper/5wbw6sr4ppzaz",
  "venue": "Astronomy & Astrophysics",
  "versions": []
}