NBYM 2006

A major proton event of 2005 January 20:

propagating supershock or superflare?

V. Grechnev1, V. Kurt2, A. Uralov1, H.Nakajima3, A. Altyntsev1, L.

Kashapova1, N. Meshalkina1 et al.

1Institute of Solar-Terrestrial Physics, Irkutsk2Moscow State University, Moscow

3Nobeyama Radio Observatory, Nobeyama

The event of 2005 January 20

Speedest (>5000 km/s) CME ever registered with LASCO @ 4.4R (06:54 UT)

Protons >700 cm-2s-1sr-1

with E>100 MeV came soon

GLE of 277 %, largest in the 23th cycle

-ray emission X7.1/2B Microwave flux ~ 105 sfu SXR

Protons

Problem in question Gopalswamy et al. (2005, 29th ICRC,

101): common shock origin for type II radio bursts and GLEs

Simnett (2006, A&A 445, 715): CME was not responsible for the relativistic ion acceleration

¿Where high-energy protons were accelerated?

Available data The event observed in X-rays and -rays:

Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI)

non-imaging Solar Neutron and Gamma spectrometer (SONG) on board CORONAS-F spacecraft from 06:43:30 on

-rays up to 100 MeV TRACE in 1600 Å line from 06:53:30 on Nobeyama Radio Polarimeters (NoRP) No NoRH observations (too late)

HXR and -ray time profiles

TRACE

RHESSISONG

HXR and -ray time profiles

RHESSI/HXR & SXR, TRACE 1600 Å

Background: TRACE 1600 Å. No images between 06:18 and 06:52:30

Red: RHESSI SXRBlue: RHESSI

HXR (50-100 kev?)

GOES/SXI:

Movie: http://svs.gsfc.nasa.gov/vis/a000000/a003100/a003161/

Comparison of TRACE 1600 Å and HXR 50-100 keV images

One can expect correlation of bright kernels in TRACE 1600 Å and HXR

This can be used for coalignment The interval of 06:52:30-06:57 Variance and averaged images

06:52 06:5706:47

Ribbons in TRACE 1600 Å images

Variance map

Time profiles

Averaged image

Outcome from TRACE 1600 Å images:

8 bright kernels at the outer parts of ribbons

4 regions with well-pronounced counterparts 4 loops: Formation of a usual (low) arcade

Try to compare with RHESSI 50-100 keV images

Comparison of 1600 Å and HXR bright kernels

White: 50-100 keV kernels Black: 1600 Å kernels Bottom: shift +7.5, -10.5 satisfactory coalignment

Now we can find relative positions of sunspots, ribbons, and X-ray sources

Relative positions of sunspots, ribbons, and X-ray sources

Ribbons crossed sunspots Large SXR loop-like structure

White Light

6-12 keV

50-100 keV

1600 Å ribbon

50-100 keV RHESSI images

N-footpoint fixed S-footpoint moves

eastwards HXR are weaker

from N-footpoint BN-foot > BS-foot,

N-footpoint needs more counterparts

N

S

Evolution of AR 10720 Magnetograms:

one week of SOHO/MDI observations, Jan 12-20

All images “co-rotated” to Jan 15, 00 UT

B > 2000 G in N-polarity sunspot

B = 1800 G

overturn

NoRP dataNote: Y scales in 103 sfu

Stokes I

Stokes V

Source A

Source B

NoRP spectra

peak, GHz

Flu

x,

10

3

sfu

Frequency , GHz

NoRP data suggest

Source A: 35 GHz < peak < 80 GHz in N-sunspot, B > 2000 G

Source B: peak < 35 GHz in S-polarity region, first in weaker sunspot, then moved eastwards

One or two more sources in weaker magnetic fields -(0.6-1.3) 1.8-2.5

Microwave emission was produced by large amount of hard electrons in strong magnetic fields

Source BSource A

SXR GOES data

Loop: h=50 Mm, l=2.6 Mm, d=0.9 Mm, V=8·1027 cm3

Neupert effect & trapping:

GOES 12

GOES 10

GOES/SXI

300-800 keV

34 GHz

17 GHz

d/dt(GOES 1-8 Å)

Ne

T

EM

Features of the event Long bundle of loops rooted in

sunspots Trapping & harder microwaves large

mirroring expectable in a large loop Many accelerated particles (estimated

from microwave fluxes) Strong magnetic fields

HXR & -ray images and spectrum

= 2.7 – softer than microwaves suggest

Nuclear lines 0.51 & 2.2 MeV

All images are confined to the active region

Ground-Level Enhancement

Perfect coincidence No dispersion with respect

to -rays Delay of ~380 s Solar wind disturbed (ACE:

~800 km/s) - path length longer

Leading edge was a bunch of ultrarelativistic protons

Conclusion 2.2 MeV line is due to collisions of MeV-energy

protons with dense layers The 2.2 MeV source image is located in region of

closed magnetic structures Protons from remote outer source have no

access into the closed structures in AR

Protons could be accelerated only in AR

On the other hand, protons accelerated in the current sheet are injected both down and up, and the latter reach the Earth to produce GLE

Was this event exceptional?

Date Peak 35 GHz 80 GHz Protons GLE Position Flare L&B Gopal1990-04-15 02:59 19615 No data N32E57 X1.41990-05-21 22:14 37913 29083 + + N35W36 X5.5 + 1991-03-22 22:44 122522 12469 + S26E28 X9.4 + 1991-03-29 06:45 10871 2196 ? S28W60 X2.41991-05-18 05:13 20429 3376 ? N32W85 X2.81991-06-04 03:41 131163 165816 + N30E65 X12 + 1991-06-06 01:08 130439 186980 + N33E44 X12 + 1991-06-09 01:38 73994 23630 + N34E04 X10 + 1991-06-11 02:05 45671 10025 + + N31W17 X12 + 1991-10-24 02:38 33967 10637 S15E60 X2.11992-11-02 02:49 41312 12000 + 15% S23W90 X9 + 2001-04-02 21:47 24952 15600 Weak 1% N17W78 X202002-07-23 00:30 14821 6000 S13E72 X4.82002-08-24 01:00 11477 4300 + 5% S02W81 X3.1 +2005-01-20 06:46 84500 50000 + 277% N14W61 X7.1 +2000-11-08 23:28 weak weak strong N20W66 M7.4 + 2001-04-18 02:14 48 + 14% S23W92 C2.2 +2001-12-26 05:05 764 111 + 7% N07W62 M7.1 +

F35 > 104 sfu 15 of 649 events

Summary High-energy protons in 2005 January 20 event

were accelerated on the Sun, within the active region

2005 January 20 event was a major proton flare

Moreover, it was a typical major proton flare

Microwave emission in such events is generated by large number of electrons with hard spectrum in strong magnetic fields

We acknowledge

Shibasaki San and NSRO for the opportunity to work here under perfect conditions

Staff members of the NSRO for the hospitality