太陽電波の長期多波長観測と地球上層大気
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1 太 陽 電 波 の 長 期 多 波 長 観 測 と 地 球 上 層 大 気 柴 崎 清 登 野 辺 山 太 陽 電 波 観 測 所 2014/03/13 研 1
2 概 要 日 本 における 太 陽 電 波 フラックス 観 測 相 対 黒 点 数 と 電 波 フラックスの 相 関 電 波 放 射 機 構 と 太 陽 大 気 太 陽 活 動 とコロナ 加 熱 Blind Source Separation 法 による 解 析 各 Sourceの 物 理 的 意 味 各 Sourceと 地 球 上 層 大 気 の 相 関 まとめ 2014/03/13 研 2
3 Solar Radio Observations in Japan (Toyokawa / Nobeyama) Total flux and polarization measurements at: 1.0, 2.0, 3.75, 9.4, 17, 35 and 80 GHz longest observation is at 3.75 GHz since Nov Robust absolute calibration (1.0 ~ 9.4 GHz) Data use (open use through INTERNET) studies of particle accelerations in solar flares (0.1 second data) index of solar activity (daily data) /03/13 IUGONET2014@STE 研 3
4 Nobeyama Radio Polarimeters 2014/03/13 研 4
5 1 AU Corrected Monthly Mean Flux (SFU) 450 Microwave Flux (1951 Nov June) & Sunspot Number GHz 3.75GHz 2.0GHz 1.0GHz Spot/ Prepared by K. Shibasaki July 25, /03/13 IUGONET2014@STE 研 5
6 Correlation between 3.75GHz Flux (NBYM) and Sunspot Number(ISN/SIDC) 2014/03/13 研 6
7 Correlation Coefficient between Sunspot Number and Microwave Flux Frequency (GHz) Wavelength (cm) Correlation Coefficient (r) ~10cm (3 GHz) fluxes show the highest correlation. Weather and ionospheric influences are minimal around 10 cm. 2014/03/13 IUGONET2014@STE 研 7
8 Radio Emission Mechanisms from the Sun Microwave (frequncy=1 ~ 10 GHz, wavelength= 30~3 cm) accelerated motion of electrons (classical EM theory) collision with ions (Coulomb force, f-f emission) gyration around magnetic field (Lorenz force, gyro-resonance emission, gyro-synchrotron emission) f-f emission Hot and dense plasma in the upper atmosphere (corona, transition region, chromosphere) gyro-resonance emission Thermal electrons gyration around very strong sunspot magnetic field (2 nd or 3 rd harmonics) gyro-synchrotron emission Non-thermal (accelerated in solar flares) electrons gyrating around active region magnetic field (higher harmonics, 2014/03/13 IUGONET2014@STE 研 8
9 Radio brightness temperature and integrated flux F T k T b 2k Id 2 d, T d d d F : flux density (W/m B b Te : Boltzmann constant, : wavelengt h, : brightness temperature, : solid angle, T : plasma temperature, : optical depth, : absorptioncoefficien t B b 2 /Hz), I : brightness, n 3/ 2 (cm ) : thermal : constant (0.1in the choromosphere, 0.2 in the corona) 2 f 2 T -1 f - f 2014/03/13 IUGONET2014@STE 研 9
10 Brightness temperatures during Frequency (GHz) solar minimum period Wavelength (cm) Flux (SFU) Tb (K) , , , ,000 (A flat circular disk is assumed for Tb, by neglecting limb brightening.) Effective temperatures (Tb) are located in the Transition region. This is the reason why microwave fluxes are good indexes of solar activity or coronal / chromospheric heating rate. (Transition region works as an amplifier of solar activity.) 2014/03/13 IUGONET2014@STE 研 10
11 Solar Atmosphere Microwave emission 2014/03/13 研 11
12 Causal Chain: SSN Microwave Flux Sunspots are phenomena below the temperature minimum. Microwave emission comes from mainly transition region which is located above the temperature minimum. Hence the causal chain is the coronal / chromospheric heating mechanism. The heating rate must be proportional to magnetic flux at the photosphere. 2013/11/11 ISSIws2013@Bern 12
13 Corona / Chromosphere Photosphere Solar activity and its indexes/proxies Indexes / proxies Influences Sunspot number (Group number) Total magnetic flux Total solar irradiance Spectral solar irradiance Hα plage area Microwave flux Number of flares and CMEs Solar activity? Coronal / chromospheric Heating Interplanetary space and Heliosphere Solar wind Cosmic ray Earth upper atmosphere Magnetosphere Radiation belt Ionosphere (fof2) Stratosphere Geomagnetic activity Auroral activity Satellite drag 2013/11/11 ISSIws2013@Bern 13
14 Coronal / Chromospheric Heating Not only heating, but also temperature regulated plasma supply is required. Should work also during activity minimum. Should work also in unipolar open magnetic field regions (coronal holes, Solar Wind source). Heating rate should be proportional to magnetic flux. Should work below the corona / chromosphere 2013/11/11 ISSIws2013@Bern 14
15 長 期 多 波 長 データの 集 約 (Blind Source Separation) 長 期 多 波 長 のデータの 中 から 統 計 的 手 法 によって 少 ない 成 分 (source)を 取 り 出 し その 物 理 的 意 味 を 議 論 する 使 用 データ 豊 川 / 野 辺 山 の1.0, 2.0, 3.75, 9.4 GHz & カナダの2.8 GHz 波 長 :30, 15, 8, 3.2 & 10.7 cm すべてのデータの 揃 った 1957 年 11 月 以 降 のデータを 使 用 (20357 日 ) 1AU 補 正 をし F10.7に 0.9の 補 正 を 施 した データギャップを 埋 めた 参 考 文 献 Synoptic radio observations as proxies for upper atmosphere modelling by T. Dudok de Wit, S. Bruinsma, K. Shibasaki, J. Space Weather Space Clim, Vol. 4, A06, /03/13 IUGONET2014@STE 研 15
16 BSSの 仕 組 み すべてのデータを 行 列 で 表 現 I(t,λ):n t n λ の 行 列 n t :データ 点 数 (20,357) n λ : 測 定 波 長 点 数 (5) wavelength (5) I(t, ) V(t) data number(20357) V(t): n t n s, S(λ): n s n λ source spectrum n s :number of sources V(t)とS(λ)を 求 める(BSS) S( ) 数 少 ないsource(s)で 記 述 できるようにする noise 2014/03/13 IUGONET2014@STE 研 16
17 The EUV Sun as the superposition of elementary Suns (A&A 487, 2008) Nt=2146 Nλ= /03/13 研 17
18 電 波 スペクトルの3つのソース 2014/03/13 研 18
19 Spectral Solar Irradiance と 電 波 フラックス 及 び 各 ソースとの 相 関 2014/03/13 研 19
20 地 球 熱 圏 密 度 モデル( 衛 星 ドラッグ) Drag Temperature Model DTM2012_F10 vs DTM2012_F /03/13 研 20
21 まとめ 日 本 における 太 陽 電 波 長 期 多 波 長 観 測 電 波 データと 太 陽 活 動 のよい 相 関 太 陽 活 動 と 彩 層 コロナ 加 熱 : 太 陽 活 動 は 加 熱 率 Blind Source Separation 法 によって 太 陽 電 波 の 長 期 多 波 長 データを 解 析 して 3つのソースを 同 定 した S1( 短 波 長 ), S2(10cmピーク), S3( 長 波 長 ) S3がEUV/UVとの 相 関 がよい 熱 圏 密 度 のモデル( 衛 星 のドラッグ)にはF10よりF30 が 有 効 である(S3の 有 効 性 ) F30(1GHz 電 波 フラックス)の 観 測 の 重 要 性 2014/03/13 IUGONET2014@STE 研 21
22 END 2014/03/13 研 22
23 Diamagnetic Force In the presence of gradient of magnetic flux density (B), charged particles are pushed toward weak B region due to their magnetic moments (mirror force). This force is not included in MHD. B F L B db dr 1 B db dr kbt B 1 db dr kbt L B magnetic moment (μ=k B T/B) L B Magnetic scale length 2013/11/11 ISSIws2013@Bern 23
24 Hot plasma flows upwards Condition that upward diamagnetic force exceeds downward gravity force is: F u 2k T m g B / Fd H0 p 0LB In the solar corona H T 6 0 /100"~ ( L 1 Temperature dependent plasma upflow / L ~ 60Mm T ~ (100" T ) L B 6 B B 6 / 60Mm) H L B 0 2kBT m g p /11/11 ISSIws2013@Bern 24
25 Hot Plasma Supply in Open Field Region 5. Solar Wind 2. thermalization / dissipation 1. energy supply (wave, magnetic) 3. heat conduction? 4. evaporation / ablation? Coronal heating (1, 2) 2013/11/11 ISSIws2013@Bern 25
26 Proposal of a simple mechanism Supply of hot plasma directly from below the photosphere, where temperature is higher, through magnetic flux tubes due to diamagnetic force of each plasma particles contained in the tube. Leakage of hotter plasma inside through magnetic flux tubes. Integrated magnetic flux is proportional to number of flux tubes (~1,500G), hence the supply rate of hot plasma is proportional to integrated magnetic flux. Magnetic fields at the photosphere are concentrated as flux tubes and plasma inside tubes are isolated (dark sunspots at the photosphere where ionization degree is very low). This mechanism satisfies most of the requirements for coronal / chromospheric heating. 2013/11/11 ISSIws2013@Bern 26
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