LISA-PF radiation monitor performance during the evolution of SEP events for the monitoring of test-mass charging

Grimani, C.; Ao, Xianzhi; Fabi, Michele; Laurenza, M.; Li, G; Lobo, Alberto; Mateos, I.; Storini, M.; Verkhoglyadova, O. P.; Zank, G. P.

doi:10.1088/0264-9381/31/4/045018

Cited by 8 publications

(5 citation statements)

References 43 publications

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“…The average matter thickness surrounding the coronagraph was set to 1.2 g/cm 2 of aluminium-honeycomb and CFRP. The projections of SEP event occurrence were carried out according to the Nymmik model (see Grimani et al 2014, and references therein). All details are reported by Telloni et al (2016a).…”

Section: Metis Radiation Environmentmentioning

confidence: 99%

Metis: the Solar Orbiter visible light and ultraviolet coronal imager

Antonucci

Romoli

Andretta

et al. 2020

A&A

141

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Aims. Metis is the first solar coronagraph designed for a space mission and is capable of performing simultaneous imaging of the off-limb solar corona in both visible and UV light. The observations obtained with Metis aboard the Solar Orbiter ESA-NASA observatory will enable us to diagnose, with unprecedented temporal coverage and spatial resolution, the structures and dynamics of the full corona in a square field of view (FoV) of ±2.9 • in width, with an inner circular FoV at 1.6 • , thus spanning the solar atmosphere from 1.7 R to about 9 R , owing to the eccentricity of the spacecraft orbit. Due to the uniqueness of the Solar Orbiter mission profile, Metis will be able to observe the solar corona from a close (0.28 AU, at the closest perihelion) vantage point, achieving increasing out-of-ecliptic views with the increase of the orbit inclination over time. Moreover, observations near perihelion, during the phase of lower rotational velocity of the solar surface relative to the spacecraft, allow longer-term studies of the off-limb coronal features, thus finally disentangling their intrinsic evolution from effects due to solar rotation. Methods. Thanks to a novel occultation design and a combination of a UV interference coating of the mirrors and a spectral bandpass filter, Metis images the solar corona simultaneously in the visible light band, between 580 and 640 nm, and in the UV H i Lyman-α line at 121.6 nm. The visible light channel also includes a broadband polarimeter able to observe the linearly polarised component of the K corona. The coronal images in both the UV H i Lyman-α and polarised visible light are obtained at high spatial resolution with a spatial scale down to about 2000 km and 15000 km at perihelion, in the cases of the visible and UV light, respectively. A temporal resolution down to 1 second can be achieved when observing coronal fluctuations in visible light. Results. The Metis measurements, obtained from different latitudes, will allow for complete characterisation of the main physical parameters and dynamics of the electron and neutral hydrogen/proton plasma components of the corona in the region where the solar wind undergoes the acceleration process and where the onset and initial propagation of coronal mass ejections (CMEs) take place. The near-Sun multi-wavelength coronal imaging performed with Metis, combined with the unique opportunities offered by the Solar Orbiter mission, can effectively address crucial issues of solar physics such as: the origin and heating/acceleration of the fast and slow solar wind streams; the origin, acceleration, and transport of the solar energetic particles; and the transient ejection of coronal mass and its evolution in the inner heliosphere, thus significantly improving our understanding of the region connecting the Sun to the heliosphere and of the processes generating and driving the solar wind and coronal mass ejections. Conclusions. This paper presents the scientific objectives and requirements, the overall optical design of the Metis instrument, t...

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Section: Metis Radiation Environmentmentioning

confidence: 99%

Metis: the Solar Orbiter visible light and ultraviolet coronal imager

Antonucci

Romoli

Andretta

et al. 2020

A&A

141

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“…A maximum number of three intense events is expected during the second half of 2015 [18]. The radiation monitor aboard LISA-PF will allow us to follow the dynamics of SEP events, including the possibility to estimate the solar particle spatial distribution [23]. In the following, we show that the LISA-PF particle detector data can be also used to study the GCR flux variations characterized by minimum periodicities of 30 min or 1 h on the basis of the GCR intensity that will be observed after the launch of LISA-PF.…”

Section: Introductionmentioning

confidence: 99%

LISA Pathfinder test-mass charging during galactic cosmic-ray flux short-term variations

Grimani

Fabi

Lobo

et al. 2015

Class. Quantum Grav.

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Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder (LPF), meant for subsystems diagnostics, was devoted to the measurement of galactic cosmic-ray and solar energetic particle integral fluxes above 70 MeV n −1 up to 6500 counts s −1. PD data were gathered with a sampling time of 15 s. Characteristics and energy-dependence of GCR flux recurrent depressions and of a Forbush decrease dated August 2, 2016 are reported here. The capability of interplanetary missions, carrying PDs for instrument performance purposes, in monitoring the passage of interplanetary coronal mass ejections (ICMEs) is also discussed.

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“…These transient solar eruptions are more frequent around solar maximum, with on average a few a year energetic enough to enhance test mass charging, but less than one a year at solar minimum. Their properties are event specific but can temporarily increase the proton flux by several orders of magnitude for durations spanning hours up to several days [5,12,13]. Given the FIG.…”

Section: The Interplanetary Charged Particle Environmentmentioning

confidence: 99%

Measuring the Galactic Cosmic Ray flux with the LISA Pathfinder radiation monitor

Armano

Audley

Baird

et al. 2018

Astroparticle Physics

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Test mass charging caused by cosmic rays will be a significant source of acceleration noise for spacebased gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor made in situ measurements of the cosmic ray flux while also providing information about its energy spectrum. We describe the monitor and present measurements which show a gradual 40% increase in count rate coinciding with the declining phase of the solar cycle. Modulations of up to 10% were also observed with periods of 13 and 26 days that are associated with co-rotating interaction regions and heliospheric current sheet crossings. These variations in the flux above the monitor detection threshold (≈ 70 MeV) are shown to be coherent with measurements made by the IREM monitor on-board the Earth orbiting INTEGRAL spacecraft. Finally we use the measured deposited energy spectra, in combination with a GEANT4 model, to estimate the galactic cosmic ray differential energy spectrum over the course of the mission.

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LISA-PF radiation monitor performance during the evolution of SEP events for the monitoring of test-mass charging

Cited by 8 publications

References 43 publications

Metis: the Solar Orbiter visible light and ultraviolet coronal imager

Metis: the Solar Orbiter visible light and ultraviolet coronal imager

LISA Pathfinder test-mass charging during galactic cosmic-ray flux short-term variations

Measuring the Galactic Cosmic Ray flux with the LISA Pathfinder radiation monitor

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