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PoS(ICRC2021)1299 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ 1 ONLINE 푐, event/flare for a solar flare which 1 − 10 × 5 . 8 and and Shintaro Ito 1 푏, Yuuki Nakano ∗ , 1 푎, event/flare would be predicted for the other side (visible side). To minimize background 4 [email protected], [email protected], − 10 × International Cosmic Ray Conference (ICRC 2021) Presenter For the Super-Kamiokande Collaboration. 36 . 1 ∗ th , Higashi-Mozumi 456, Kamioka-cho, Hida-city, Gifu, 506-1205, Japan Kobe University, Department of Physics, Kobe, Hyogo, 657-8501, Japan KEK, 1-1 Oho, Tsukuba, Ibaraki, 305-0801,E-mail: Japan [email protected] Importance of search for generated during solar flares hashowever, neutrinos been discussed associated for last with 60 years, solar flares (solarSince flare neutrinos) neutrinos have are not been not obserbedprovide yet. affected us by with information interplanetary about magnetic ato field, particle some acceleration theoretical solar mechanism predictions, flare in fluxenergy neutrinos solar and of flares. the would the location According where solar solar flare flaresof ocurr detection on by would the Super-Kamiokande depend (SK) surface. detector on Typicaloccurs is predicted the on probability releasing the opposite side1 of Sun surface from the (invisible side). On the other hands, for the solar flare neutrino searches,analyzed data and of time solar windows satellites for (GOES,Coronal solar RHESSI, Mass Ejection and flare event Geotail) neutrino catalogs were were searchesneutrinos used on on to the the determine invisible side the visible of search the sidedetector. windows Sun. were for SK solar The defined. is flare the SK world’s largest experiment undergroundresults has water of Cherenkov been solar flare started neutrino the searches using measurement data of sets neutrinos from SK-I since to 1996. SK-IV are presented. The Copyright owned by the author(s) under the terms of the Creative Commons 푐 푎 푏 © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 37 July 12th – 23rd, 2021 Online – Berlin, Germany Kohei Okamoto, Search for neutrinos associated with solar flare PoS(ICRC2021)1299 Kohei Okamoto 4 5 6 − − − 10 10 10 85 × . 7.5 × × 0.75 0 0 8 36 . . . 9 3 1 event in SK [/flare] The number of expected 2 isotropic isotropic isotropic isotropic beam like beam like generation condition 휈 - - 1 3 1 Summary of the predicted solar flare models. 3 – 4 Power index of parent Table 1: Model Ref. [3] Ref. [4] Ref. [5] MeV. Therefore, the most interested energy region for solar flare neutrino event is [4]. For Fargion’s and Moscato’s prediction [5], the neutrino flux was estimated MeV, which typically overlapped with the energy range of atmospheric neutrinos [6] 70 − 500 MeV), pions are produced by collisions with other nuclei in the solar atmosphere [1]. et al. − 50 10 300 Since neutrinos are generated via the decay of charged pions, the energy spectra have peak There are mainly three predictions for solar flare neutrino flux at the Earth with different Solar flares convert magnetic energy into plasma heating and the kinetic energy ofNeutrinos charged associated with solar flares (solar flare neutrinos) attract significant attention in the and Supernova Relic Neutrinosatmospheric (SRNs) neutrinos is [7]. technically difficult because ofatmospheric the The same neutrinos production separation mechanism. are between Although constantly solar generated, flare solar flare neutrinos neutrinos and are expected to be released 2. Search Time Window for Neutrinos around from assumptions. The flux of solarin flare solar neutrinos depends flares on which theflare appear condition neutrinos of as was the power proton simulated index acceleration assumingproton of the acceleration isotropic proton with (visible the energy side) Monte distribution.Takeishi and Carlo methods beam-like Generation by (invisible Kocharov, side) of Kovaltsov, and solar Usoskin [3], and Finally, neutrinos are generated via the decayatmospheric of neutrinos. those charged Because pions of through this hadronic thethe origin, same solar acceleration processes flare as of neutrinos give information about aslast well 60 years, as solar subsequent flare neutrinos interactions have inbut been experimentally not the sought observed by solar yet. several . neutrino detectors [2] For the using the amount of energyis taken assumed up that by pion the production amountprotons out are of of headed energy for the carried the total solar away energyexpected surface event varies of or observed by depending the solar the solar Super-Kamiokande on flares. (SK) atmosphere. detector whether in The It in the each1. conditions Table prediction accelerated and are summarized the number of particles such as protons.interact Protons with the injected dense downwards plasma from in the the coronal lower solar acceleration atmosphere. region will field of astrophysics. If protons are acceleratedthan during solar flares to sufficiently high energies (more Search for neutrinos associated with solar flare 1. Introduction PoS(ICRC2021)1299 ] 2 − 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 cm 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 10 [ - × × × × × × × × × × × × × × × × × × × × × × Kohei Okamoto 6 6 6 6 6 6 6 6 6 6 6 5 6 6 6 6 6 6 6 6 9 6 ...... 5 5 5 5 5 5 5 5 5 5 5 8 5 5 5 5 5 5 5 5 8 5 HIGHE 90 Fluence limit Φ ------(UTC) 19:42:26 12:03:05 Event time 1 MeV MeV 8 9 . . No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal No signal 181 No SK data 1186 observed signal Visible energy of 3 End (UTC) 11:54:58 10:28:31 21:52:57 19:21:31 13:51:03 16:33:38 14:31:05 00:31:36 08:36:03 11:10:57 20:50:07 17:26:03 19:56:03 06:57:12 17:39:48 21:08:05 21:20:36 10:35:43 18:47:06 08:05:40 00:25:16 12:03:20 16:06:32 Start (UTC) 00:04:21 11:54:39 15:49:12 14:24:25 00:25:08 08:20:32 10:59:30 20:38:46 17:12:01 19:36:59 06:39:22 17:23:34 21:00:27 19:13:00 10:24:18 18:41:29 08:00:50 11:52:13 10:08:44 21:35:10 19:12:32 13:43:48 16:28:36 S13E72 S21E88 S16E08 S11E77 S12E75 S12E67 S07E68 S05E64 S21E83 S21E31 S17E34 N22E12 N16E09 S09W34 S08W88 S15W02 S14W56 S19W83 S18W63 S20W85 N14W61 N14W69 N22W07 AR location X5.4 X9.4 X8.3 X5.3 X5.1 X5.4 X9.2 X7.1 X5.4 X6.2 X9.0 X6.5 X7.4 X9.5 X5.7 X5.6 X5.8 Class X17.2 X10.0 X28.0 X18.2 X20.0 X14.4 2 Summary of solar flares used for the search. The date, class and active region (AR) location Date As described in Sec.1, the predicted neutrino flux originated from the solar flares occurred on To search for solar flare neutrinos from visible side of the Sun, the public data from solar It was a period of reconstructionIt work was of failed to SK. obtain thetime time window window is determined set by derivative by of using soft soft X-ray X-ray for time this profile. solar flare. Further discussion For this can flare, be the found search in Ref. [11]. 2017 Sep. 6 2005 Sep. 7 2005 Sep. 8 2005 Sep. 9 2001 Apr. 2 2001 Apr. 6 2003 Nov. 2 2003 Nov. 4 1997 Nov. 6 2006 Dec. 5 2006 Dec. 6 2012 Mar. 7 2002 Jul. 23 2000 Jul. 14 2011 Aug. 9 2005 Jan. 20 2003 Oct. 28 2003 Oct. 29 2003 Oct. 23 2017 Sep. 10 2001 Apr. 15 1 2 2001 Dec. 13 2001 Aug. 25 2.2 The Invisible Side Solar Flares the invisible side would be larger than that of visible side. To obtain the information of solar flares are taken from a National Oceanicinformation is and written Atmospheric in Administration Universal source Time (NOAA Coordinate [12]). (UTC). All time satellites GOES [8], RHESSI [9]for and Integrated GEOTAIL Data [],10 Science (CIDAS) and at computational Nagoyawith University resources were more used. of than the In X5.0 Center this study,23. class the solar were The flares selected solar and flaresdetermined are the summarized using number in of the2. Table solar timedetailed The flares profile method. time used of of for soft the the start X-ray analysis derivative and is end using ofTable GOES, 2: each see flare Ref. were [11] for more Search for neutrinos associated with solar flare only during the time scale of particleneutrinos) acceleration to in background solar (atmospheric flare. neutrinos) can Thus, betime the improved window. ratio by of setting For signal an this (solar appropriate purpose, flare search neutrinos we by firstly using set the the data search recorded time bysolar the windows flare for satellites. neutrinos searching After were for sought the solar determination using flare of the the SK time data windows, taken from2.1 April 1996 to Solar May Flares 2018. on the Visible Side PoS(ICRC2021)1299 ] 2 − 5 5 6 5 6 5 5 5 ). Based cm 10 10 10 10 10 10 10 10 [ 휎 - - × × × × × × × × 6 6 2 6 2 2 2 6 ...... 5 5 1 5 1 8 8 5 HIGHE 90 Fluence limit Kohei Okamoto Φ ) before the CMEs 휎 ------(UTC) 15:18:34 15:40:45 13:07:36 14:15:21 22:09:37 03:03:47 Event time 1 1 MeV MeV MeV MeV MeV MeV 9 3 6 1 5 8 ...... No signal No signal No signal No signal 493 125 834 No SK data No SK data 3555 1351 2135 observed signal Visible energy of End 4 (UTC) 03:16:02 20:07:58 17:14:12 10:10:01 16:41:57 07:07:35 14:45:29 22:52:20 03:19:45 15:07:12 Start (UTC) 20:51:42 01:19:07 13:06:34 01:15:24 18:07:20 15:13:34 08:09:23 14:41:19 05:06:57 12:44:51 E90b E90b E90b W90b SW90b SW90b S15E90 S17W132 S20W143 N16W153 AR location [km/s] 2425.5 2003.2 2221.6 2464.2 2191.3 2046.6 2036.0 2237.0 2008.1 2527.8 CME speed Summary of solar flares occurred on the invisible side. The date, CME speed and location SK is a water Cherenkov detector located at 1,000 m (2,700 m water equivalent) below the top The high-energy data sample has three different categories: fully contained (FC) neutrinos, At first, we selected 10 CMEs occurred on the invisible side of the Sun, whose speed exceeds Date It was a period of reconstruction work of SK. 2011 Jun. 4 2003 Nov. 7 2003 Nov. 9 2003 Nov. 2 2005 Jul. 24 2012 Jul. 23 2002 Jul. 19 2002 Jul. 20 2001 Apr. 18 1 2014 Dec. 13 3. Analysis of Super-Kamiokande Data of Mt. Ikenoyama in Gifuusing the prefecture, analysis tools Japan in [17]. SK. The energy Searchabove region of and for this below solar analysis are 100 flare divided into MeV neutrinos two (High-energyand energy was regions, data background performed sample rate of and each low-energy sample data are sample). summarized in The4. Table 3.1 livetime High-energy Data Sample partially contained (PC) neutrinos,detailed information and of upward-going the event muon categories.peak (UPMU). of In expected See this energy spectrum study, Ref. the ofof [18] FC solar the data flare FC for neutrinos sample sample more is is was 100 around used MeV 70 since to MeV, the and 10 the GeV. energy range 2000 km/sec. This criterionstatistical roughly evaluation corresponds [15]. to In theflares addition, solar is flare also the examined with difference and class of the X2.0 the standard according deviation start of to time its between distribution CMEs is and 1020 seconds solar (1 Search for neutrinos associated with solar flare on the invisible side, Coronal Mass Ejectionsurface (CME) of data the was used. invisible side Although the iswith states not CME on observed data the directly, solar recorded the by startintensity LASCO time and [14]. of CME speed. solar There flares is can weak be positive estimated correlation between solar flare on this study, we setemission. the For start the time end time, of we thein conservatively used Subsection search2.1 4178since window seconds all determined as processes from (acceleration, 3060 X-ray energycomplete described seconds release within and (3 etc) this occurs time during a duration. solarin flare The3. Table solar flares occurred on the invisible side are summarized Table 3: are taken from SOHO LASCOCoordinate (UTC). CME catalog [16]. All time information is written in Universal Time PoS(ICRC2021)1299 Kohei Okamoto event/day event/day event/day event/day 01 02 01 01 . . . . 0 0 0 0 ± ± ± ± 20 19 20 19 . . . . 0 0 0 0 background event rate Low energy data sample livetime 794 days 562 days 1497 days 2970 days events) for solar flare event on November 29 . 0 . Further information about the reconstruction event/day event/day event/day event/day 1 5 07 09 12 05 . . . . 0 0 0 0 ± ± ± ± events ( 45 33 53 48 . . . . 7 7 7 7 background event rate 58 . 0 Summary for SK data set High energy data sample livetime 825 days 522 days 1489 days 3235 days Table 4: Jun. 2001 May 2018 Oct. 2005 Sep. 2008 − − − − Data period event/flare. It is the same for all the solar flares on the invisible side since the search Jul. 2006 62 Oct. 2002 Apr. 1996 Sep. 2008 . 0 There is no signal in low-energy data sample while six events in high-energy data sample The number of neutrino candidate events observed in the search window can be converted to There is no signal detected in low energy data sample while two events in the high energy data Low-energy data sample can be categorized into two data sets, solar neutrino data [19] and The solar angle cut was used for the SRNs searches, however, this cut was not used for the solar flare neutrino SK-I 1 SK-II SK-III SK-IV SK Phase analysis. as summarized in3. Table time3 Figure windowshows described the in energybackground Sec2. and energy time2 Figure spectrum. of(right) observedsample shows The is events the expected with energy number search of of observed background event events with of the high-energy data the upper limit on thecalculated neutrino using the fluence. Fagion’s and Moscat’s In prediction. this The study, 90% the C.L. limits limits on of the the fluence solar of flare solar neutrinos were 4th 2003 (September 6thconsistent 2017). with background. The probability of no signal event4.2 is 32.2% Invisible (21.8%) Side Solar which Flares is time range is uniform for thesearch flares window on are the two invisible eventsThe for side. probabilities the The of solar numbers flares no of on signalcases, observed November event but 7th events for they in 2003 these are and consistent solar July with flares 24th background. 2005. are 10.2%. These4.3 are the most Fluence extreme limit using Fagion’s and Moscat’s Model 4. Result 4.1 Visible Side Solar Flares sample detected as summarized inwith2. Table light curves1 Figure recordedshows by thebackground GOES. time energy2 Figure of(left) spectrum. observed shows events thesamples together The energy in of expected the observed search number event time of with windows is the background events of high-energy data methods and event selection can be found in Kirk et al. [7]. SRNs data [7]. Therange SRNs data of were the used SRNs for the data solar is flare from neutrino analysis 16 because to the 100 energy MeV Search for neutrinos associated with solar flare 3.2 Low-energy Data Sample

PoS(ICRC2021)1299 Soft X-ray [Count] X-ray Soft (1) (2) 3 10 7000 6000 5000 4000 3000 2000 1000 0 × 7000 09/06 12:04 6000 Visible Energy[MeV] Visible 09/06 12:02 Time (UTC) Time Kohei Okamoto 5000 right: 15:18:34 right: 14:15:21 left: 15:40:45 left: 13:07:36 Nov. 7th 2003 Nov. Jul. 24th 2005 22:09:37 Jun. 4th 2011 Jul. 23rd 2012 03:03:47 Background Spectrum 09/06 12:00 )) 푖 Solar flares on invisible side 휈 4000 09/06 11:58 퐸 ( is 2.30 for all flare events. 휖 ) 09/06 11:56 ) 푖 3000 90 휈 휈 푁 퐸 퐸 ( ( Soft X-ray Derivative of Soft X-ray Neutrino event time (12:03:05 Sep. 6 2017) 09/06 11:54 휖 휎 2000 ) ) + 푖 . 푒 휈 09/06 11:52 Solar flare on Sep. 6 2017 Solar flare on Sep. 6 퐸 3 , 퐸 ( 1000 10 flare 휈 × 퐹 0 / 09/06 11:50 40 30 20 10 80 70 60 50 퐸 ( 2

(

− 6 Derivative of soft X-ray [Counts/s] X-ray soft of Derivative 1 0 90 / 휎 90 0.8 1.2 0.6 0.4 0.2 ) 1

푁

cm 푁 Event/Search time window time Event/Search 휈 ¯ 휏 7 퐸 ¯ 휇, ( 6 10 ¯

푒,

퐹 Soft X-ray [Count] X-ray Soft 휈 × is the number of target proton in SK relevant to the 퐸 7 3 . 푝 d 푒,휇,휏, 10 1 5000 7000 6000 5000 4000 3000 2000 1000 0 × = 푁 ∫ 푖 11/04 20:00 푝 Í 4500 푁 휈 퐸 4000 [MeV] Energy Visible = d Time (UTC) Time ∫ 3500 푇 LOWE 90 Nov. 4th 2003 19:42:26 Nov. Sep. 6th 2017 12:03:05 Background Spectrum 푁 3000 11/04 19:50 Φ Soft X-ray Derivative of Soft X-ray Neutrino event time 4 2003) (19:42:26 Nov. is the Invers Beta Decay (IBD) cross section which is used in event = Solar flare on visible side 2500 The detector on GOES was saturated 휎 Solar Flare on Nov. 4th 2003 Solar Flare on Nov. HIGHE 90 2000 Φ 1500 11/04 19:40 1000 is the 90% C.L. limit of the observed neutrino events calculated with a Poisson distribution 3 Left (right) plot is energy spectra of background and observed events in search time window of Neutrino event timing on soft X-ray light curve and its time derivative recorded by GOES. Green 10 500 × 90 0 70 60 50 40 30 20 10 80 푁 0

1

For the high energy data set, the fluence limit of solar flare neutrino can be obtained using the 0.8 Derivative of Soft X-ray [Count/s] X-ray Soft of Derivative 0.2 0.6 0.4 1.2 Event/Search time window time Event/Search equation Assuming the energy spectrum of solarfluence flare limit neutrino for the is low Fargion’s and energy Moscat’s sample prediction is [5], the Figure 1: square (Red point) shows countneutrino rate event of timing. soft Gray X-ray band (time isdue derivative to corresponding of saturation to soft of search X-ray). photon time detector window. Black on The dashed GOES flat line from count shows 19:43:18 rate to on 19:56:51 left on plot November is 4th 2003. neutrino interactions, simulaition. Since there was no signal in low energy data samples, Figure 2: Search for neutrinos associated with solar flare solar flare on visible (invisible)blue side. and orange Red lines histogram show shows the backgroundrespectively. energies energy of spectrum. the neutrino Green, events in magenta, search time windows from each solar flare, neutrinos can be calculated using the following equation where with the number of background events, PoS(ICRC2021)1299 (3) 07/24 00:00 Time(UTC) 07/25 11:00 Time(UTC) 07/23 23:00 Kohei Okamoto 07/25 10:00 is the combined Neutrino events Estimated CME start time Neutrino events Estimated CME start time 07/23 22:00 휎 Jul. 23rd 2012 July. 24th 2005 July. 07/25 09:00 07/23 21:00 07/25 08:00 ) 휈 07/23 20:00 퐸 ( 07/25 07:00 휖 ) 07/23 19:00 + 푒 07/25 06:00 , 퐸 07/23 18:00 휈 07/25 05:00 퐸 ( 07/23 17:00 휎 ) 07/25 04:00 90 휈 3 3 4 4 푁 퐸 10 10 10 10

−

Visible Energy [MeV] Energy Visible Visible Energy [MeV] Energy Visible 7 퐸 ( 훿 휈 퐸 d 11/08 13:00 Time(UTC) Time(UTC) 06/05 19:00 ∫ 푝 11/08 12:00 푁 06/05 18:00 Neutrino events Estimated CME start time Neutrino events Estimated CME start time = Jun. 4th 2011 Nov. 7th 2003Nov. ) 11/08 11:00 06/05 17:00 퐸 ( 11/08 10:00 90 06/05 16:00 Φ 11/08 09:00 06/05 15:00 is delta function and other variables are same as that in Eq. (1). The same 11/08 08:00 ) 06/05 14:00 휈 퐸 11/08 07:00 − 06/05 13:00 is the number of target nuclei relevant to the neutrino interactions, Time distribution of neutrino events in high energy data sample for solar flares on invisible side. 퐸 푇 ( 11/08 06:00 12:00 06/05 훿 푁 3 3 4 4

10 10 10 10 To compare the results of this work with the other experimental results, the model independent For solar flares on the visible and invisible sides, we estimated the time of neutrino emission

Visible Energy [MeV] Energy Visible Visible Energy [MeV] Energy Visible fluence upper limit was also calculated for the low energy sample using the equation procedure laid out in Ref.upper [20] limits was of used fluence to for calculate solarKamiokande-II flare the result, neutrinos values. the with4 Figure model sensitivity independentshows was method. the improvedfrom by results 20 Comparing an of to to order the 110 the of MeV. magnitude in the energy region 5. Summary and discussion from optical and CME observations, respectively. Then,with we the searched for solar neutrino events flares associated inside Super-Kamiokande. and six Two neutrino neutrino eventsare events from background from consistent, solar solar so flares flares the on on upper the limit the of invisible visible the side solar are flare observed, neutrino but fluence is all calculated. of them The cross section for all interactions.in The the 90% high C.L. energy upper data limits(invisible sample of side). in the Assuming fluence each that the for flare search solar are timetime flare windows summarized are in neutrino sufficient in solar to2 cover Table flares, the(visible the neutrino emission fluence side) limit and does3 Table not depend4.4 on the duration Model of independent search fluence time upper window. limit where Figure 3: Red points show neutrinocorresponding event to in estimated start SK. time Grey of band CME emission. shows the search time window.where Black dashed line is Search for neutrinos associated with solar flare PoS(ICRC2021)1299 , , 61 4(S257) :2105.02458. Kohei Okamoto Astropart. Phys. arXiv Phys. Rev. Lett. , 417. : 2014, 14 .: 2021, .: 1988, et al. , 3. et al et al , 239. , 75. energy e , 2. 3 ν 100 33 210 ) , 3656. e ν 36 Nuvo Cim. C 2013 80 , 418. , 344. SK Upper Limit (This work) Kamland ES+IBD ( Kamiokande , 034501. 501 , date last accessed July 1 2021. , 1-2, pp. 357-402. Solar Phys. 2812 78 60 , 102001. , L4. 8 162 , 10. , 13.; Hirata, K.S., , 344. ; Aharmim, B., , 112005. 103 , 052007. 857 , 072001. , 052010. 32 71 295 40 :1909.02422. ; Abe, S., , date last accessed July 1 2021. 382 85 97 94 Proc. SPIE. APJ arXiv Chin. J. Astron. Astrophys. 20 Solar Phys. Annu. Rev. Astron. Astrophys. Rev. Sci. Instrum. Proceedings of the International Astronomical Union Solar Phys. Geophysical Research Letters Proceedings of 33rd ICRC 0 .: 1991, Nucl. Instrum. Meth. A .: 2019, Phys. Rev. Lett. 9 8 7 Phys. Rev. Lett. 11 15 13 14 12 10 .: 1995, 10 10 10 Phys. Rev. Lett. 10 10 10 10 10 10 Phys. Rev. Lett. Phys. Rev. Lett. Astrophys. J. Lett.

et al Fluence (/flare) [cm (/flare) Fluence ] et al -2 .: 2020, .: 2007b, et al .: 2008, . : 2009, .: 2013, Prog. Part. Nucl. Phys. : 2021, .: 2003, .: 2005, et al et al .: 2012, et al .: 2018, .: 2016, .: 2018, et al et al et al et al. et al et al et al et al et al Model independent upper limit for solar flare neutrino search. Red solid line shows the upper , 1. ; Agostini, M., https://www.ngdc.noaa.gov/stp/space-weather/solar-data/solar-features/ solar-flares/x-rays/goes/xrs/ https://cdaw.gsfc.nasa.gov/CME_list/ 2653. ; Aglietta, M., ;Abbasi, R, 233-243. 55 [2] Davis, R.: 1994, [4] Takeishi, R., [5] Fargion, D., Moscato, F.:[6] 2003, Abe, K., [7] Kirk, B., [8] Hanser, F.A., Sellers, F.B.:[9] 1996, Lin, R.P., Dennis, B.R., Hurford, D.M.: 2002, [3] Kocharov, G.E., Kovaltsov, G.A., Usoskin, I.G.: 1991, [1] Hudson, H., Ryan, J.: 1995, [10] Tanaka, Y.T., [11] Okamoto, K., [17] Fukuda, S., [12] Solar flare catalog based on data recorded by GOES, available at [16] CME catalog based on data recorded by LASCO, available at [18] Ashie, Y., [19] Abe, K., [13] Davies, J.A., [14] Brueckner, G. E., [15] Yashiro, S., [20] Abe, K., obtained result is the strongdate. constraint More of detailed the analysis fluence is of on-going solar and the flare results neutrinos are in presentedReferences MeV in region the up future to publication. Figure 4: limit calculated from this result.result [2]. Black dotted (Orange dashed) line shows the Kamiokande (KamLAND) Search for neutrinos associated with solar flare