Lessons learnt from the STEREO Heliospheric. Imagers: Tracking

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Presentation transcript:

Lessons learnt from the STEREO Heliospheric. Imagers: Tracking Lessons learnt from the STEREO Heliospheric Imagers: Tracking & modelling CMEs from Sun to Earth Richard Harrison Jackie Davies Chris Davis Chris Eyles Steve Crothers

The heritage Coronagraphs (OSO, Skylab, SMM, P78-1, SOHO, STEREO) Helios photometers SMEI (Coriolis) Coronal Mass Ejections (CMEs) – Discrete solar ejecta, ‘typically’ 1012 to 1013 kg of matter expelled at a few 100 kms-1. The challenge: Identify and predict the impact of Earth-directed CMEs.

STEREO Concept

Heliospheric Imager Concept: Wide-angle imager with occultation & baffle system; light rejection of ~ 10-13 of the solar brightness. Consortium: RAL, University of Birmingham, CSL and NRL Principal elements of the design: CFRP structure and baffles, CCD wide-angle camera system, passive cooling, one-shot door, mounted on side of spacecraft Harrison et al., 2008, Solar Phys. 247, 171 Eyles et al., 2009, Solar Phys. 254, 387

Door Radiator HI-1 Side & rear baffles Door latch mechanism HI-2 Inner Baffles Forward Baffles Direction of Sunlight

< 0.1 CME intensity at inner edge of FOV Launch – Oct 26 2006; Doors opened – Dec 13 2006 (HI-A) & Jan 11 2007 (HI-B); Scientific Operations – from Apr 2007 HI-1 HI-2 Direction of Centre of FOV 14 degrees 53.7 degrees Angular Field of View 20 degrees 70 degrees Angular Range 4-24 degrees 18.7-88.7 degrees Image Array (2x2 binning) 1024x1024 Image Pixel Size 70 arcsec 4 arcmin Spectral Bandpass 630-730 nm 400-1000 nm Nominal Image Cadence 40 min 120 min Brightness Sensitivity (Bo = solar disk) 3 x 10-15 Bo 3 x 10-16 Bo Straylight Rejection 3 x 10-13 Bo 10-14 Bo < 0.1 CME intensity at inner edge of FOV ~ magnitude 12; governed by anticipated CME intensity at outer edge [Adapted from Socker et al.]

You are here! Smile – we are photographing you every 2 hours!

The events of 7 March 2012

The view from STEREO A

Apparent acceleration at large elongations – the ‘Fixed Phi’ approximation HI pixels Elongation angle φ Sun A Ho~1AU Time (Sheeley et al., JGR,1999) Assuming the CME propagates radially (φ constant) and at a constant speed; (φ) (φ)

Geometrical models: (a) Fixed Phi (Alexis Rouillard et al.) – open ‘dots’ (a) Harmonic Mean (Noe Lugaz, Christian Möstl et al.) – filled ‘dots’ (b) Self Similar Expansion (Jackie Davies et al.) [λ: 0 = FP; 90 = HM]

(Davies et al., 2012)

Triangulation: Self Similar Expansion model using two viewpoints (Davies et al. in prep)

Points to note: Only scratched the surface! (Forward modelling, Variable speeds, hybrid codes, drag, deflection, CME-CME interaction, also: CIRs, comets...) No other instrument has ever imaged CMEs approaching & running over Earth in this way Note! STEREO is a science mission: the spacecraft continue to drift Given the importance of understanding & predicting CMEs, this demonstration is ripe for using in an operational scenario (one spacecraft or two; L4/L5; <60o etc...)

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