The Solar Mass Ejection Imager (Smei)

Eyles, C. J.; Simnett, G. M.; Cooke, M. P.; Jackson, B. V.; Buffington, A.; Hick, P. P.; Waltham, Nicholas R.; King, Julien; Anderson, Peter; Holladay, P. E.

doi:10.1023/b:sola.0000006903.75671.49

Cited by 232 publications

(197 citation statements)

References 4 publications

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“…Using a combination of the Solar Mass Ejection Imager (SMEI) archive and Liverpool Telescope SkyCamT 1 observations Hounsell et al (2010) confirmed that KT Eri was already in outburst on A&A 537, A34 (2012) 2009 November 13.12 and constrained the time of maximum to 2009 November 14.67 ± 0.04 (which we take as t = 0). The band pass for the SMEI is from 4500−9500 Å with a peak quantum efficiency of the instrument at 7000 Å (Eyles et al 2003). Hounsell et al (2010) also reported a significant pre-maximum halt before the luminosity peaked at m SMEI = 5.42 ± 0.02 and confirmed the very fast nature of the outburst (t 2 = 6.6 days).…”

Section: Introductionmentioning

confidence: 73%

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

Jurdana-Šepić

Ribeiro

Darnley

et al. 2011

A&A

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Context. Nova Eridani (2009) caught the eye of the nova community due to its fast decline from maximum, which was initially missed, and its subsequent development in the radio and X-ray wavelengths. This system also exhibits properties similar to those of the much smaller class of recurrent novae; themselves potential progenitors of type Ia supernovae. Aims. We aim to determine the nature and physical parameters of the KT Eri progenitor system. Methods. We searched the Harvard College Observatory archive plates for the progenitor of KT Eri to determine the nature of the system, particularly the evolutionary stage of the secondary. We used the data obtained to search for any periodic signal and the derived luminosity to estimate a recurrence timescale. Furthermore, by comparing the colours of the quiescent system on a colour−magnitude diagram we may infer the nature of the secondary star. Results. We identified the progenitor system of KT Eri and measured a quiescent magnitude of B = 14.7 ± 0.4. No previous outburst was found. However, we suggest that if the nova is recurrent it should be on a timescale of centuries. We find a periodicity at quiescence of 737 days which may arise from reflection effects and/or eclipses in the central binary. The periodicity and the quiescence magnitude of the system suggest that the secondary star is evolved and likely in, or ascending, the Red Giant Branch. A second period is evident at 376 days which has a sinusoidal like light curve. Furthermore, the outburst amplitude of ∼9 mag is inconsistent with those expected for fast classical novae (∼17 mag) which may lend further support for an evolved secondary. Conclusions. We investigated the probable recurrent nova KT Eri for which we suggest an inter-outburst period of order centuries and an evolved secondary. This may suggest that there is a whole range of possible inter-outburst periods in between the "typical" classical and recurrent novae nomenclature. Archival searches are an excellent tool in order to investigate the nature of astrophysical objects, in order to determine the nature and physical parameters.

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Section: Introductionmentioning

confidence: 73%

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

Jurdana-Šepić

Ribeiro

Darnley

et al. 2011

A&A

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“…This technique required considerable interpretation and projection but it is clear that CMEs were detected successfully out of the Sun -Earth line. A recent major advance was made with the launch of the Solar Mass Ejection Imager (SMEI) aboard the Coriolis spacecraft, in 2003 (Eyles et al, 2003). This instrument maps the entire sky with three cameras, each scanning 60-degree slices of the sky as the spacecraft moves around the Earth.…”

Section: Relevant Space Instrumentationmentioning

confidence: 99%

First Imaging of Coronal Mass Ejections in the Heliosphere Viewed from Outside the Sun – Earth Line

et al. 2007

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We show for the first time images of solar coronal mass ejections (CMEs) viewed using the Heliospheric Imager (HI) instrument aboard the NASA STEREO spacecraft. The HI instruments are wide-angle imaging systems designed to detect CMEs in the heliosphere, in particular, for the first time, observing the propagation of such events along the SunEarth line, that is, those directed towards Earth. At the time of writing the STEREO spacecraft are still close to the Earth and the full advantage of the HI dual-imaging has yet to be realised. However, even these early results show that despite severe technical challenges in their design and implementation, the HI instruments can successfully detect CMEs in the heliosphere, and this is an extremely important milestone for CME research. For the principal event being analysed here we demonstrate an ability to track a CME from the corona to over 40 degrees. The time -altitude history shows a constant speed of ascent over at least the first 50 solar radii and some evidence for deceleration at distances of over 20 degrees. Comparisons of associated coronagraph data and the HI images show that the basic structure of the CME remains clearly intact as it propagates from the corona into the heliosphere. Extracting the CME signal requires a consideration of the F-coronal intensity distribution, which can be identified from the HI data. Thus we present the preliminary results on this measured F-coronal intensity and compare these to the modelled F-corona of Koutchmy and Lamy (IAU Colloq. 85, 63, 1985). This analysis demonstrates that CME material some two orders of magnitude weaker than the F-corona can be detected; a specific example at 40 solar radii revealed CME intensities as low as 1.7×10 −14 of the solar brightness. These observations herald a new era in CME research as we extend our capability for tracking, in particular, Earth-directed CMEs into the heliosphere.

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“…This heliospheric imaging capability built on the heritage of the Solar Mass Ejection Imager instrument on the Coriolis spacecraft (Eyles et al 2003). The STEREO mission is comprised of two spacecraft, with one leading (STEREO A) and the other trailing (STEREO B) the Earth in its orbit.…”

Section: Thomson Scattering Wl Formulaementioning

confidence: 99%

Using Coordinated Observations in Polarized White Light and Faraday Rotation to Probe the Spatial Position and Magnetic Field of an Interplanetary Sheath

Xiong

Davies

Feng

et al. 2013

ApJ

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Coronal mass ejections (CMEs) can be continuously tracked through a large portion of the inner heliosphere by direct imaging in visible and radio wavebands. White light (WL) signatures of solar wind transients, such as CMEs, result from Thomson scattering of sunlight by free electrons and therefore depend on both viewing geometry and electron density. The Faraday rotation (FR) of radio waves from extragalactic pulsars and quasars, which arises due to the presence of such solar wind features, depends on the line-of-sight magnetic field component B and the electron density. To understand coordinated WL and FR observations of CMEs, we perform forward magnetohydrodynamic modeling of an Earth-directed shock and synthesize the signatures that would be remotely sensed at a number of widely distributed vantage points in the inner heliosphere. Removal of the background solar wind contribution reveals the shock-associated enhancements in WL and FR. While the efficiency of Thomson scattering depends on scattering angle, WL radiance I decreases with heliocentric distance r roughly according to the expression I ∝ r −3 . The sheath region downstream of the Earth-directed shock is well viewed from the L4 and L5 Lagrangian points, demonstrating the benefits of these points in terms of space weather forecasting. The spatial position of the main scattering site r sheath and the mass of plasma at that position M sheath can be inferred from the polarization of the shock-associated enhancement in WL radiance. From the FR measurements, the local B sheath at r sheath can then be estimated. Simultaneous observations in polarized WL and FR can not only be used to detect CMEs, but also to diagnose their plasma and magnetic field properties.

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The Solar Mass Ejection Imager (Smei)

Cited by 232 publications

References 4 publications

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

First Imaging of Coronal Mass Ejections in the Heliosphere Viewed from Outside the Sun – Earth Line

Using Coordinated Observations in Polarized White Light and Faraday Rotation to Probe the Spatial Position and Magnetic Field of an Interplanetary Sheath

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