White light flares trace and rhessi observations
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White-Light Flares: TRACE and RHESSI Observations. H. Hudson (UCB), J. Wolfson (LMSAL) & T. Metcalf (CORA). White-Light Flares (WLF). “White light” is formed deep in the solar atmosphere and is therefore energetically important (also note “white-light prominences,” which are up in the corona)

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White-Light Flares: TRACE and RHESSI Observations

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White light flares trace and rhessi observations

White-Light Flares: TRACE and RHESSI Observations

H. Hudson (UCB), J. Wolfson (LMSAL)

& T. Metcalf (CORA)


White light flares wlf

White-Light Flares (WLF)

  • “White light” is formed deep in the solar atmosphere and is therefore energetically important (also note “white-light prominences,” which are up in the corona)

  • White-light (and UV) continuum emission associates well, at least in part, with the hard X-ray impulsive phase (Neidig)

  • There are some WLF observations from space prior to TRACE (Yohkoh; Matthews et al., 2003), but TRACE and RHESSI give us much better data

  • Solar-B should be able to make wonderful observations of WLF


Event selection

Event Selection

  • TRACE catalog => events with <10 s cadence in white light and full resolution, GOES C and above, full RHESSI coverage

  • Total event list consists of 33 events during RHESSI operations through 2004

  • 11 events (X: 0; M: 7; C: 4)

  • All 11 events have TRACE WL response

  • All 11 events have RHESSI hard X-ray response

  • 10/11 events appear to be largely footpoints; one has obvious coronal sources as well


White light flares trace and rhessi observations

TRACE spectral

Response

Solar-cycle modulation

(Lean, 1997)


Event list a

Event Lista

aHudson et al., Solar Phys. (in press, 2005)


White light flares trace and rhessi observations

2002 Oct. 4

05:35:49 UT

2002 Oct. 5

10:41:58 UT


White light flares trace and rhessi observations

WL versus UV (1700A)

TRACE WL

WL difference

1700 A


White light flares trace and rhessi observations

Intermittency

32 x 68 arc s frames


White light flares trace and rhessi observations

WL-1700A Comparison

Reversed colors!


White light flares trace and rhessi observations

WL-hard X-ray comparison


Conclusions

Conclusions

  • WL emission, as seen by TRACE, is not resolved at angular resolution 1”, temporal resolution 10 s

  • The data confirm a strong association with hard X-rays

  • Sources may be extended in area and include loop tops

  • “True” WL is morphologically different from UV

    • TRACE WL contrasts can exceed 100% even for flares below X class


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