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Ion Acceleration in Solar Flares Determined by Solar Neutron Observations 2013 AGU Meeting of the Cancun, Mexico 2013/05/15 Kyoko Watanabe ISAS/JAXA,

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Presentation on theme: "Ion Acceleration in Solar Flares Determined by Solar Neutron Observations 2013 AGU Meeting of the Cancun, Mexico 2013/05/15 Kyoko Watanabe ISAS/JAXA,"— Presentation transcript:

1 Ion Acceleration in Solar Flares Determined by Solar Neutron Observations 2013 AGU Meeting of the Americas @ Cancun, Mexico 2013/05/15 Kyoko Watanabe ISAS/JAXA, Japan and the Solar Neutron Observation Group

2 Solar Flare Magnetic reconnection model There is limited information regarding particle acceleration － electron acceleration: radio, hard X-rays － ion acceleration: lineγ-ray, solar neutron Information about ion acc. can be obtained from the foot-points Solar neutrons are produced by the interaction of accelerated ions with the ambient solar atm. near the solar surface We can get the information of ion acceleration from solar neutron

3 Solar neutron observation Solar neutron Propagation Attenuation Detector ⇒ ⇒ ⇒ Sun Atmosphere Ground Neutron - Neutron monitor - Solar neutron telescope Detector ・ γ-ray Solar flare Ion acceleration

4 Solar Neutron Events DateTime [UT]ObservatoryX-ray classSunspot loc. 1982/06/03 11:43JungfraujochX 8.0S09 E72 1990/05/24 20:48ClimaxX 9.3N36 W76 1991/03/22 22:44HaleakaraX 9.4S26 E28 1991/06/04 03:37NorikuraX12.0N30 E70 1991/06/0600:58 Japan, Hawaii X12.0N33 E44 2000/11/2414:51 Chacaltaya X 2.3N22 W07 2001/08/2516:23 Chacaltaya X12.0S17 E34 2003/10/2809:51 Tsumeb X17.4S16 E08 2003/11/0217:03 Chacaltaya X 8.3S14 W56 2003/11/0419:29 Hawaii X28.0S19 W83 2005/09/0717:17 Bolivia, Mexico X17.0S06 E89

5 Solar neutron event on 2005 Sep 7 ObservatoryAir mass Chacaltaya, Bolivia612 g/cm 2 Sierra Negra, Mexico603 g/cm 2 Mexico City, Mexico825 g/cm 2 39.4σ 8.7σ 15.5σ 11.9σ

6 INTEGRAL & RHESSI γ–ray data on 2005 Sep 7 INTEGRAL 200 – 300 keV RHESSI 4.4 MeV 2.2 MeV C : 4.4MeV

7 Hua’s model (Hua et al., 2002) – Physical parameters – loop length pitch-angle scattering magnetic convergence ambient composition atmospheric model flare heliocentric angle – Acceleration parameters – acceleration release time history spectrum (power-law spectral index) accelerated ion composition

8 Neutron Spectrum for 2005 Sep 7 event The power law index of escape neutrons to the Earth is estimated from proton index, and obtained as -3.1. We explain observed long-time neutron emission by using γ-ray profile as ion acceleration profile. (Watanabe et al., 2009) λ= 5000 δ= 0.20 s = -3.6 L = 38,600 km E c = 400 MeV The predicted neutron profile was well fit to the observed data when the proton index is -3.6.

9 Solar Neutron Events Date Time [UT] ObservatoryX-ray class Sunspot loc. 1982/06/0 3 11:43JungfraujochX 8.0S09 E72 1990/05/2 4 20:48ClimaxX 9.3N36 W76 1991/03/2 2 22:44HaleakaraX 9.4S26 E28 1991/06/0 4 03:37NorikuraX12.0N30 E70 1991/06/0 6 00:58 Norikura, Hawaii X12.0N33 E44 2000/11/2 4 14:51 Chacaltaya X 2.3 N22 W07 2001/08/2 5 16:23 Chacaltaya X12.0S17 E34 2003/10/2 8 09:51 Tsumeb X17.4S16 E08 2003/11/0 2 17:03 Chacaltaya X 8.3S14 W56 2003/11/0 4 19:29 Hawaii X28.0S19 W83 2005/09/0 7 17:17 Bolivia, Mexico X17.0S06 E89

10 Date Flare class Observatory Power index Flux @ 100MeV [/MeV/sr] 1982/06/03X8.0 Jungfraujoc h –4.0±0.2(2.6±0.7)×10 28 1990/05/24X9.3Climax–2.9±0.1(4.3±0.4)×10 28 1991/03/22X9.4Haleakala–2.7±0.1(6.0±1.0)×10 26 1991/06/04X12.0Norikura–4.9±0.6(1.9±0.2)×10 27 1991/06/06X12.0Norikura–4.1±1.0----------- 2000/11/24X2.3Chacaltaya–4.2±0.5(4.0±1.3)×10 26 2001/08/25X5.3Chacaltaya–3.1±0.4(2.4±1.3)×10 26 2003/10/28X17.4Tsumeb–3.8±0.4(3.7±1.4)×10 27 2003/11/02X8.3Chacaltaya–7.0±1.3(2.8±1.6)×10 26 2003/11/04X28Haleakala–3.9±0.5(1.5±0.6)×10 28 2005/09/0717:17 Chacaltaya -3.1----------- Neutron energy spectra Neutron index α n = –3 ～ –4

11 Date Flare class Observatory Neutron power index Proton index 1982/06/03X8.0Jungfraujoch–4.0–5.0 1990/05/24X9.3Climax–2.9–3.8 1991/03/22X9.4Haleakala–2.7–3.5 1991/06/04X12.0Norikura–4.9–6.0 1991/06/06X12.0Norikura–4.1–5.1 2000/11/24X2.3Chacaltaya–4.2–5.2 2001/08/25X5.3Chacaltaya–3.1–4.0 2003/10/28X17.4Tsumeb–2.9–3.8 2003/11/02X8.3Chacaltaya–6.1–7.4 2003/11/04X28Haleakala–3.6–4.6 2005/09/0717:17 Chacaltaya –3.1–3.6 Proton spectra of solar neutron events

12 Solar Neutron Events Date Time [UT] ObservatoryX-ray class Sunspot loc. 1982/06/0 3 11:43JungfraujochX 8.0S09 E72 1990/05/2 4 20:48ClimaxX 9.3N36 W76 1991/03/2 2 22:44HaleakaraX 9.4S26 E28 1991/06/0 4 03:37NorikuraX12.0N30 E70 1991/06/0 6 00:58 Norikura, Hawaii X12.0N33 E44 2000/11/2 4 14:51 Chacaltaya X 2.3 N22 W07 2001/08/2 5 16:23 Chacaltaya X12.0S17 E34 2003/10/2 8 09:51 Tsumeb X17.4S16 E08 2003/11/0 2 17:03 Chacaltaya X 8.3S14 W56 2003/11/0 4 19:29 Hawaii X28.0S19 W83 2005/09/0 7 17:17 Bolivia, Mexico X17.0S06 E89

13 Flare position of solar neutron events Solar Cycle 21, 22 Solar Cycle 21, 22, 23 Limb flare : >60 deg Solar Cycle 21, 22 3 Limb flare 2 Disk flare Solar Cycle 21, 22, 23 5 Limb flare 6 Disk flare There is no correlation between solar neutron event and flare position

14 0° 89° neutron Solar flare model needs to explain the mechanism to accelerate ions or to produce neutrons away from the solar surface ⇒ (Hua & Lingenfelter, 1987) Solar neutrons are easier to be observed from limb flares rather than disk flares

15 Summary – Observation Results Until now, 11 solar neutron events in association with large solar flares were observed by the ground based detectors. Intense emission of γ -rays was observed by satellite. Solar neutrons are produced with γ -rays. Neutron spectra ⇒ α n = –3.0 ～ –4.0 Proton index is softer by about 1 than neutron index ⇒ α p = –4.0 ～ –5.0 There is no correlation between the longitude of solar flares and solar neutron events ⇒ direction of ion acceleration New solar neutron detectors Space Environment Data Acquisition equipment–Attached Payload (SEDA-AP) in ISS SciBar for the Cosmic Ray Telescope (SciCRT)

16 Solar neutron Detector: SEDA-AP SEDA-AP: Space Environment Data Acquisition equipment– Attached Payload (SEDA-AP) SEDA- FIB BBD detector (<30MeV) FIB detector (30-120MeV)

17 2009.12.03 23:59:59UT background neutron Typical example of observed neutron signal We have searched for solar neutrons in association with all flares with an intensity higher than M-class, and have found some neutron signals from some flares. We still working on many solar flares for to find neutron signal Solar neutron Detector: SEDA-AP

18 Solar neutron Detector: SciCRT http://stelab.nagoya-u.ac.jp/ste-www1/div3/CR/Neutron/ SciBar for the cosmic ray telescope – Can measure the energy of the solar neutrons – Can measure arrival directions – Located at Mt. Sierra Negra in Mexico

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