Magnetic field investigation of the Venus plasma environment: Expected new results from Venus Express

Zhang, T.L.; Baumjohann, W.; Delva, M.; Auster, H. U.; Balogh, A.; Russell, C. T.; Barabash, S.; Balikhin, M. A.; Berghofer, G.; Biernat, H. K.; Lämmer, H.; Lichtenegger, H.; Magnes, W.; Nakamura, R.; Penz, T.; Schwingenschuh, K.; Vörös, Z.; Zambelli, W.; Fornaçon, K.‐H.; Glaßmeier, K.‐H.; Richter, Ingo; Carr, C.; Kudela, K.; Shi, Jian; Zhao, Hu; Motschmann, U.; Lebreton, Jean‐Pierre

doi:10.1016/j.pss.2006.04.018

Cited by 239 publications

(195 citation statements)

References 38 publications

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“…The arrival time correction for VEX is already about 30 hr at this longitudinal separation. In Figure 5, we show B measured by VEX in Venus solar orbital coordinates (Zhang et al 2006), but rotated by 180 • (B x = −B xVSO ; B y = −B yVSO ) so it approximately matches the RTN coordinates orientation we used for STEREO-B. We linearly interpolated over time intervals when VEX was below three Venus radii to see only the solar wind magnetic field.…”

Section: Stereo-b Vex and Ace In Situ Observationsmentioning

confidence: 99%

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

Möstl

Rollett

Lugaz

et al. 2011

ApJ

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One of the goals of the NASA Solar TErestrial RElations Observatory (STEREO) mission is to study the feasibility of forecasting the direction, arrival time, and internal structure of solar coronal mass ejections (CMEs) from a vantage point outside the Sun-Earth line. Through a case study, we discuss the arrival time calculation of interplanetary CMEs (ICMEs) in the ecliptic plane using data from STEREO/SECCHI at large elongations from the Sun in combination with different geometric assumptions about the ICME front shape [fixed-Φ (FP): a point and harmonic mean (HM): a circle]. These forecasting techniques use single-spacecraft imaging data and are based on the assumption of constant velocity and direction. We show that for the slow (350 km s −1 ) ICME on 2009 February 13-18, observed at quadrature by the two STEREO spacecraft, the results for the arrival time given by the HM approximation are more accurate by 12 hr than those for FP in comparison to in situ observations of solar wind plasma and magnetic field parameters by STEREO/IMPACT/PLASTIC, and by 6 hr for the arrival time at Venus Express (MAG). We propose that the improvement is directly related to the ICME front shape being more accurately described by HM for an ICME with a low inclination of its symmetry axis to the ecliptic. In this case, the ICME has to be tracked to >30 • elongation to obtain arrival time errors <± 5 hr. A newly derived formula for calculating arrival times with the HM method is also useful for a triangulation technique assuming the same geometry.

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Section: Stereo-b Vex and Ace In Situ Observationsmentioning

confidence: 99%

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

Möstl

Rollett

Lugaz

et al. 2011

ApJ

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“…23 in Brace and Kliore, 1991). Estimates of the total solar wind induced oxygen ion escape from Venus range from the order of 10 24 s −1 to 10 26 s −1 including observational and simulation studies (e.g., Brace et al, 1987;Moore and McComas, 1992;Terada et al, 2004;Lammer et al, 2006;Kallio et al, 2006b;Barabash et al, 2007a;Martinecz et al, 2009). We select to call the value 10 25 s −1 as the nominal O + escape rate.…”

Section: Introductionmentioning

confidence: 99%

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions

et al. 2009

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Abstract. We study the solar wind induced oxygen ion escape from Venus' upper atmosphere and the Venus Express observations of the Venus-solar wind interaction by the HYB-Venus hybrid simulation code. We compare the simulation to the magnetic field and ion observations during an orbit of nominal upstream conditions. Further, we study the response of the induced magnetosphere to the emission of planetary ions. The hybrid simulation is found to be able to reproduce the main observed regions of the Venusian plasma environment: the bow shock (both perpendicular and parallel regions), the magnetic barrier, the central tail current sheet, the magnetic tail lobes, the magnetosheath and the planetary wake. The simulation is found to best fit the observations when the planetary O + escape rate is in the range from 3×10 24 s −1 to 1.5×10 25 s −1 . This range was also found to be a limit for a test particle-like behaviour of the planetary ions: the higher escape rates manifest themselves in a different global configuration of the Venusian induced magnetosphere.

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“…We now apply the above methods to the magnetic field data from the Venus Express (VEX) spacecraft (Zhang et al, 2006) in orbit around the planet Venus. The signal represents a sample of the x component of the solar wind magnetic field, measured by VEX on 17 January 2007.…”

Section: Satellite Data Testsmentioning

confidence: 99%

Effect of data gaps: comparison of different spectral analysis methods

et al. 2016

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Abstract. In this paper we investigate quantitatively the effect of data gaps for four methods of estimating the amplitude spectrum of a time series: fast Fourier transform (FFT), discrete Fourier transform (DFT), Z transform (ZTR) and the Lomb-Scargle algorithm (LST). We devise two tests: the single-large-gap test, which can probe the effect of a single data gap of varying size and the multiple-small-gaps test, used to study the effect of numerous small gaps of variable size distributed within the time series. The tests are applied on two data sets: a synthetic data set composed of a superposition of four sinusoidal modes, and one component of the magnetic field measured by the Venus Express (VEX) spacecraft in orbit around the planet Venus. For single data gaps, FFT and DFT give an amplitude monotonically decreasing with gap size. However, the shape of their amplitude spectrum remains unmodified even for a large data gap. On the other hand, ZTR and LST preserve the absolute level of amplitude but lead to greatly increased spectral noise for increasing gap size. For multiple small data gaps, DFT, ZTR and LST can, unlike FFT, find the correct amplitude of sinusoidal modes even for large data gap percentage. However, for in-situ data collected in a turbulent plasma environment, these three methods overestimate the high frequency part of the amplitude spectrum above a threshold depending on the maximum gap size, while FFT slightly underestimates it.

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Magnetic field investigation of the Venus plasma environment: Expected new results from Venus Express

Cited by 239 publications

References 38 publications

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions

Effect of data gaps: comparison of different spectral analysis methods

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Magnetic field investigation of the Venus plasma environment: Expected new results from Venus Express

Cited by 239 publications

References 38 publications

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

ARRIVAL TIME CALCULATION FOR INTERPLANETARY CORONAL MASS EJECTIONS WITH CIRCULAR FRONTS AND APPLICATION TOSTEREOOBSERVATIONS OF THE 2009 FEBRUARY 13 ERUPTION

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O&lt;sup&gt;+&lt;/sup&gt; ions

Effect of data gaps: comparison of different spectral analysis methods

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Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions