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Contraction of flaring loops — the evidence of magnetic reconnection in sheared core fields. Haisheng Ji Purple Mountain Observatory Nanjing, 210008, China [email protected]. What is the Contraction of flaring loops?. - PowerPoint PPT Presentation
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Contraction of flaring loops — the evidence of magnetic reconnection in sheared core fields
Haisheng JiPurple Mountain ObservatoryNanjing, 210008, [email protected]
What is the Contraction of flaring loops?
That is, during the rising phase of solar flares, hard X-ray (HXR) loop-top sources or radio/extreme-ultraviolet (EUV) flaring loops have a descending motion and, at the same time, Hα ribbons or HXR footpoints (FPs) are converging. The usual expansion motion (upward motion + separation motion) of flaring loops occurs only after the contraction.
Unshearing occurs during the contraction as well as the expansion motion.
Dynamic flaring loops— A Summary from our observations
• 中国古代天文学家对太阳黑子的描述,大体可分为三大类:• 第一类,圆形:如钱、如桃、如李、如栗、如环。• 第二类,椭圆形:如鸡卵、鸭卵、鹅卵、爪、枣。• 第三类,不规则形:如立人、如踆乌、如飞鹊、如飞燕。
• 《淮南子•精神训》载:“日中有踆乌,而月中有蟾蜍。”东汉高诱注云:“踆,犹‘蹲’也,谓三足乌。”晋代学者郭璞( 276 ~ 324 )也有注释说“中有三足乌”。
Events showing the contraction
• The M1.2 flare of 2002-04-15 (Sui & Holman 2003)• The M2.1 flare of 2002-09-09 (Ji et al. 2004)• The X3.1 flare of 2002-08-24 (Li & Gan 2005)• The X3.9 flare of 2003-11-03 (Veronig et al. 2006)• The M1.2 flare of 2004-11-01 (Ji et al. 2006)• The M6.8 flare of 2003-06-13 (Ji, Huang, & Wang 2007)• The M5.7 flare of 2002-03-14 (Zhou, Ji & Huang 2006)• The X10 flare of 2003-10-29 (Zhou, Ji & Huang 2006; Ji et al. 2008)
in the early phase of the flares, the looptop sources moves down
Velocity ~ tens of kilometers per second
10-25 keV
The M1.2 flare of 2002-04-15(Sui and Holman 2003)
the first SMESE workshop 10-12 March 2008, Paris
The X3.1 flare of 2002-08-24
(Li and Gan 2005)
the first SMESE workshop 10-12 March 2008, Paris
The M3.9 flare of 2003-11-03
(Veronig et al. 2006)
the first SMESE workshop 10-12 March 2008, Paris
The M2.1 flare of 2002-09-09 (Ji et al. 2004)
Red: 6-12keVBlue: 12-25kev
25-50 keV
25 km/s
17:41 UT
17:46UT
The M1.2 flare of 2004-11-01: (Ji et al. 2006)
03:18:44 – 03:18:56
03:19:08 – 03:19:20 Solid: 25-60 keVDashed: 6-10 keV
the first SMESE workshop 10-12 March 2008, Paris
The M6.8 flare of 2003-06-17 (Ji et al. 2007)
The flare of 2002-03-14(Zhou et al. 2007)
Background: TRACE 171 AContours: HXR 30-60 keV
the first SMESE workshop 10-12 March 2008, Paris
• White-light flare (Xu et al. 2004)
• Penumbral decay and rapid magnetic changes (Wang et al. 2004)
• Gamma-ray (Hurford et al. 2006)
• Large scale disturbance (Liu et al. 2006; Balasubramaniam, Pevtsov \& Neidig 2007)
• Shear flows (Deng et al. 2006)
• Magnetic unshearing after flare (Wang et al. )
• Significant helicity drop after flare (Liu et al. 2007)
• Significant geophysical effect (Kwabara et al. 2004)
• Contraction-to-expansion (Zhou et al. 2007)
The X10 flare of 2003-10-29 (Ji et al. 2008)
10-25 keV 35-50 keV
The X10 flare of 2003-10-29 (Ji et al. 2008)
the first SMESE workshop 10-12 March 2008, Paris
The X10 flare of 2003-10-29
Sigmoid arcade
the first SMESE workshop 10-12 March 2008, Paris
The X10 flare of 2003-10-29 (Ji et al. 2008)
the first SMESE workshop 10-12 March 2008, Paris
Sigmoid phase
Arcade phase
The X10 flare of 2003-10-29 (Ji et al. 2008)
The X10 flare of 2003-10-29 (Ji et al. 2008)
the first SMESE workshop 10-12 March 2008, Paris
Contraction expansion
The X10 flare of 2003-10-29 (Ji et al. 2008)
the first SMESE workshop 10-12 March 2008, Paris
• Sigmoidal structure first ever seen in HXR• Magnetic reconnection inside the sigmoid• Sigmoid arcade • Contraction expansion • Unshearing throughout the flare• Rapid unshearing during the ‘sigmoid’ period
The X10 flare of 2003-10-29 (Ji et al. 2008)
the first SMESE workshop 10-12 March 2008, Paris
the first SMESE workshop 10-12 March 2008, Paris
Contraction of flaring loops ☆ inward motion of conjugate flaring kernels
☆ shrinkage of flaring loops (radio, EUV) ☆ descending of HXR looptop sources
Expansion of flaring loops
☆ outward motion of conjugate flare ribbons ☆ expansion of flare loops (radio, EUV)
☆ upward motion of HXR looptop sources
the first SMESE workshop 10-12 March 2008, Paris
dynamic flare loops
A B C D
E F Gthe first SMESE workshop
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dynamic flare loops
the first SMESE workshop 10-12 March 2008, Paris
Interpretation of Loop Contraction10-25 keV
1. Current sheet formation (Sui & Holman 2003, Sui et al. 2004)
2. Magnetic shrinkage (Acton & Forbes1996,
Lin 2004)
3. Collapsing magnetic trap (Veronig et al. 2005)
4. Magnetic Implosion (Hudson 2000)
V dVB )8/( 2 reducedthe first SMESE workshop
10-12 March 2008, Paris
V dVB )8/( 2
Mapping effectfrom
the Photosphere
Modifying effect caused by
Our interpretation (Ji et al. 2007)
the first SMESE workshop 10-12 March 2008, Paris
Our interpretation (Ji et al. 2007)
• Contraction is the signature of magnetic energy dissipation in highly sheared magnetic field
Energy dissipation
the first SMESE workshop 10-12 March 2008, Paris
The implication for the relationship of flares and CMEs
sigmoidal phase arcade phase
contraction expansion+
+
CMEs
the first SMESE workshop 10-12 March 2008, Paris
THANK YOU!
the first SMESE workshop 10-12 March 2008, Paris