Flare Ribbon Expansion and Energy Release Ayumi Asai Nobeyama Solar Radio Observatory, NAOJ April 6, 2005 @Nainital, India First of all, I would like the SOCs and the LOCs for inviting me and their kind arrangements. Today, I would like to present what can we learn from flare ribbon expansion.

Nobeyama Radioheliograph cadence: 1 sec spatial resolution: 10” 17 GHz / 34 GHz flare, prominence, sunspot circular polarization I belong to Nobeyama Solar Radio Observatory, National Astronomical Observatory of Japan, which is located in the middle of Japan main island. We have a radio interferometer named Nobeyama Radioheliograph. http://solar.nro.nao.ac.jp/

Flare Ribbon Expansion and Energy Release Ayumi Asai Nobeyama Solar Radio Observatory, NAOJ April 6, 2005 @Nainital, India First of all, I would like the SOCs and the LOCs for inviting me and their kind arrangements. Today, I would like to present what can we learn from flare ribbon expansion.

Solar Flare

Magnetic Reconnection Model (Carmichael 1964; Sturrock 1966; Hirayama 1974; Kopp-Pneuman 1976) well explains observed phenomena phenomenologically succeeded still needs to be checked quantitatively and qualitatively

magnetic reconnection Flare Ribbons magnetic reconnection 2001-4-10 flare (Hida Obs.) size : 104 – 105 km duration : 10 min – 10 hours Ha flare ribbons

What can we learn from Flare Ribbons? Two elongated bright regions (two ribbon) on each side of magnetic neutral line Two ribbons have the opposite magnetic polarity (N/S) to each other Two ribbons separate to each other with a speed of about several 10 km/s in earlier phase, and decelerated to about several km/s in later phase Correspond to the footpoints of post-flare loops  What can we learn from flare ribbons?

2001-April-10 Flare Flare April 10, 2001 05:10 UT GOES X2.3 NOAA 9415 East West Ha images taken with Sartorius Telescope

Observations Data Ha･･Sartorius Telescope, Kyoto University (Ha center) EUV・・TRACE (171A) HXR・・Yohkoh/HXT microwave・・ Nobeyama Radioheliograph magnetogram・・SOHO/MDI Sartorius Telescope (Kwasan Obs.)

1. Conjugacy of Ha Footpoints Nonthermal particles and thermal conduction bombard the chromospheric plasma at both the footpoints simultaneously The temporal evolution of both the footpoints is very similar(Sakao 1994) We identify the conjugated pairs of the footpoints which show similar light curves ? N S simultaneously brighten

Conjugacy of Ha footpoints divided flare ribbons into fine meshes determine “conjugated footpoints” by using cross-correlation function red:positive, blue:negative

The TRACE loops really connect the pairs. TRACE Flare Loops TRACE 171A The TRACE loops really connect the pairs. East West

Temporal evolution of Ha kernels The pairs are classified according to the times of brightening

Focus on Each Pair Movement of the site of energy release t

2. Energy Release Rate quantitative estimation of the amount of the released energy, based on the magnetic reconnection model and by using observable values  test the reconnection model Reconnection model indicates Bc : coronal magnetic field strength vin : inflow velocity A : area of the reconnection region

Energy Release Rate Electric Field  conservation of Bc : coronal magnetic field strength Bp : photospheric magnetic field strength vin : inflow velocity vf : separation speed of flare ribbons  conservation of magnetic flux It is very difficult to estimate physical values (Bc, vin) in the corona Poynting Flux I estimate the energy release rate, by using observable values (Bp, vf)

Evolution of Flare Ribbons Neutral Line B v I estimate the reconnection rate vB, and the Poynting flux vB2 as the representations of the energy release rates.

Evolution of Flare Ribbons Neutral Line B v I estimate the reconnection rate vB, and the Poynting flux vB2 as the representations of the energy release rates.

Evolution of Flare Ribbons Neutral Line B v I estimate the reconnection rate vB, and the Poynting flux vB2 as the representations of the energy release rates.

Energy Release Rate Energy Release Rate HXR sources flare ribbons Ha image Energy Release Rate We compare the derived energy release rate with HXR light curves

Reconnection Rate and Poynting Flux microwave HXR An HXR burst occurred on the slit (05:19 UT). reconnection rate Poynting flux

Reconnection Rate and Poynting Flux microwave HXR reconnection rate An HXR burst occurred on the slit (05:26 UT). Poynting flux

Quantitative Estimation W1 Comparison of Poynting and Electric Field (Reconnection Rate) between the Ha kernels with HXR sources and those without ones E2 W2 E2 W2 E1 W3 E3 E4 W4

3. Ha kernel spectroscopy Ichimoto & Kurokawa 1984 Ha spectrum flare Ha line is shifted red-ward red-asymmetry velocity : 50-100 km/s X-ray corona Ha compression chromosphere l Ha line

Red-Asymmetry Map we calculated as an indicator of r.a. all over the flare ribbon, the tendency of r.a. is seen map

Red-Asymmetry Distribution strong asymmetry @outer edges of the flare ribbon 1000~3000 km (?) at HXR sources, r.a. is not necessary strong

Scatter plot (intensity vs RA) Iblue-Ired vs r.a. scatter plot the brighter the kernel is, the stronger the r.a. is intensity of Ha kernel red blue

Summary We can learn from Ha flare ribbons: Select conjugated footpoints by calculating the cross-correlation function Estimate energy release rate, by using the separation motions of two ribbons and the photospheric magnetic field strengths Examine red-asymmetry distribution by using Ha wing data

2D / 3D observed as Ha flare ribbons

Temporal evolution of Red-Asymmetry red-asymmetry peak precedes the HXR/microwave peaks (HXR bursts are not necessary associated with strong red-asymmetry)

Scatter Plot より明るいカーネルほど、赤でより明るい red asymmetryがより強く出ていることを示唆? Haカーネルの強度 bright より明るいカーネルほど、赤でより明るい red asymmetryがより強く出ていることを示唆? dark bright in red bright in blue

Haカーネルのライトカーブ 場所によってさまざまなライトカーブを示す

Neupert Effect The shape of light curves in HXRs and microwaves correspond to the time-derivative of SXR ones! (Neupert 1968) Radiation in SXRs ~ total energy HXR/microwave radiations ~ energy release rate

Ha線での放射 非熱的粒子や熱伝導がフレアループに沿って伝播し、足元で彩層に突入する Haカーネルの増光 Haフレアリボンの形成 エネルギー解放したループの足元の場所が分かる Haフレアリボンとして観測

Haカーネルと硬X線放射源 フレア(磁気リコネクション)に伴い、硬X線で非熱的な放射源が生成 非熱的・高エネルギー粒子が彩層に突入 硬X線放射源とHaカーネルを生成 非熱的・高エネルギー粒子の彩層突入 硬X線 Ha線 コロナ 　彩層 制動放射 急激な熱化など