The Solar Mass Ejection Imager (SMEI) Mission

Jackson, B. V.; Buffington, A.; Hick, P. P.; Kuchar, T. A.; Mizuno, D. R.; Webb, D. F.

doi:10.21236/ada427103

Cited by 37 publications

(45 citation statements)

References 12 publications

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“…Webb et al 2006). Jackson et al (2004) provide the history of the smei design and development, and the instrument design and testing are described by Eyles et al (2003). A description of its performance is given in Webb et al (2006).…”

Section: Photometry From Space: Wire Smei and Hipparcosmentioning

confidence: 99%

Eclipsing binaries observed with the WIRE satellite

Bruntt¹,

Southworth²,

Torres

et al. 2006

A&A

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Context. Determinations of stellar mass and radius with realistic uncertainties at the level of 1% provide important constraints on models of stellar structure and evolution.Aims. We present a high-precision light curve of the A0 IV star ψ Centauri, from the star tracker on board the wire satellite and the Solar Mass Ejection Imager camera on the Coriolis spacecraft. The data show that ψ Cen is an eccentric eclipsing binary system with a relatively long orbital period.Methods. The wire light curve extends over 28.7 nights and contains 41 334 observations with 2 mmag point-to-point scatter. The eclipse depths are 0.28 and 0.16 mag, and show that the two eclipsing components of ψ Cen have very different radii. As a consequence, the secondary eclipse is total. We find the eccentricity to be e = 0.55 with an orbital period of 38.8 days from combining the wire light curve with data taken over two years from the Solar Mass Ejection Imager camera.Results. We have fitted the light curve with ebop and have assessed the uncertainties of the resulting parameters using Monte Carlo simulations. The fractional radii of the stars and the inclination of the orbit have random errors of only 0.1% and 0.01• , respectively, but the systematic uncertainty in these quantities may be somewhat larger. We have used photometric calibrations to estimate the effective temperatures of the components of ψ Cen to be 10 450 ± 300 and 8800 ± 300 K indicating masses of about 3.1 and 2.0 M .There is evidence in the wire light curve for g-mode pulsations in the primary star.

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Section: Photometry From Space: Wire Smei and Hipparcosmentioning

confidence: 99%

Eclipsing binaries observed with the WIRE satellite

Bruntt¹,

Southworth²,

Torres

et al. 2006

A&A

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“…Each of these cameras images a 60-by-3 degree slice of the zenith-facing hemisphere at a 4-s cadence, resulting in data on a 170-by-3 degree slice of the sky. Due to the Coriolis satellite's orbital geometry, this slice will co-rotate with the satellite over the course of an orbit such that the entire sky is imaged at an approximately 100-min cadence (Jackson et al 2004).…”

Section: Data and Light-curve Extractionmentioning

confidence: 99%

Oscillations inβ Ursae Minoris

Tarrant¹,

Chaplin²,

Elsworth³

et al. 2008

A&A

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Aims. From observations of the K4III star β UMi we attempt to determine whether oscillations or any other form of variability is present. Methods. A high-quality photometric time series of ≈1000 days in length obtained from the SMEI instrument on the Coriolis satellite is analysed. Various statistical tests were performed to determine the significance of features seen in the power density spectrum of the light curve. Results. Two oscillations with frequencies 2.44 and 2.92 µHz have been identified. We interpret these oscillations as consecutive overtones of an acoustic spectrum, implying a large frequency spacing of 0.48 µHz. Using derived asteroseismic parameters in combination with known astrophysical parameters, we estimate the mass of β UMi to be 1.3 ± 0.3 M . Peaks of the oscillations in the power density spectrum show width, implying that modes are stochastically excited and damped by convection. The mode lifetime is estimated at 18 ± 9 days.

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“…IPS observations taken using the Cambridge IPS array in the UK (Houminer, 1971), show structures that can be classified as either corotating or detached from the Sun (Gapper et al, 1982;Hewish and Bravo, 1986;Behannon, Burlaga, and Hewish, 1991). More recently, IPS data used in conjunction with tomographic threedimensional (3D) reconstruction techniques have shown the global shapes of heliospheric density and velocity structures including corotating regions and coronal mass ejections (CMEs) or their interplanetary counterparts (ICMEs) in the solar wind (see, e.g., Jackson et al, 1998;Kojima et al, 1998;Asai et al, 1998;Jackson, Hick, and Buffington, 2002;Jackson et al, 2003;Jackson and Hick, 2005;Tokumaru et al, 2007;Tokumaru, Kojima, and Fujiki, 2010;Bisi et al, 2007Bisi et al, , 2008aBisi et al, , 2008bBisi et al, , 2009aBisi et al, , 2009bJackson et al, 2008aJackson et al, , 2008bJackson et al, , 2009Jackson et al, , 2010. These tomographic analyses match in-situ spacecraft measurements from near-Earth spacecraft fairly well.…”

Section: Introductionmentioning

confidence: 99%

A Heliospheric Imager for Deep Space: Lessons Learned from Helios, SMEI, and STEREO

et al. 2010

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The zodiacal-light photometers on the twin Helios spacecraft, the Solar Mass Ejection Imager (SMEI) on the Coriolis spacecraft, and the Heliospheric Imagers (HIs) on the Solar-TErrestrial RElations Observatory (STEREO) twin spacecraft all point the way to optimizing future remote-sensing Thomson-scattering observations from deep space. Such data could be provided by wide-angle viewing instruments on Solar Orbiter, Solar Probe, or other deep-space probes. Here, we present instrument specifications required for a successful heliospheric imager, and the measurements and data-processing steps that make the best use of this remote-sensing system. When this type of instrument is properly designed and calibrated, its data are capable of determining zodiacal-dust properties, and of threedimensional reconstructions of heliospheric electron density over large volumes of the inner heliosphere. Such systems can measure fundamental properties of the inner heliospheric plasma, provide context for the in-situ monitors on board spacecraft, and enable physicsbased analyses of this important segment of the Sun-spacecraft connection.Remote Sensing of the Inner Heliosphere

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The Solar Mass Ejection Imager (SMEI) Mission

Cited by 37 publications

References 12 publications

Eclipsing binaries observed with the WIRE satellite

Eclipsing binaries observed with the WIRE satellite

Oscillations inβ Ursae Minoris

A Heliospheric Imager for Deep Space: Lessons Learned from Helios, SMEI, and STEREO

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