Short-term forecasting of solar energetic ions on board LISA

Grimani, C.; Araújo, H. M.; Fabi, Michele; Lobo, Alberto; Mateos, I.; Shaul, D.; Sumner, T. J.

doi:10.1088/1742-6596/228/1/012040

Cited by 6 publications

(7 citation statements)

References 9 publications

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“…The charging process of the free-floating proof-masses induces spurious forces that might mimic genuine gravitational wave signals in the interferometer bandwidths as it was shown in Ref. 7.…”

Section: Introductionmentioning

confidence: 77%

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Grimani

2013

Int. J. Mod. Phys. D

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Test-mass charging due to galactic cosmic rays (GCRs) and solar energetic particles (SEPs) represents one of the major sources of noise for missions devoted to gravitational wave detection in space. Particle detectors on board future space interferometers will help in monitoring the test-mass charging process. Variations and fluctuations of GCRs and evolution of SEP events of different intensities are discussed here for the correlation of SEP radiation monitor observations and particle fluxes charging the test masses. We consider the performance of the radiation monitors designed for the LISA Pathfinder mission for the results presented in this work. We point out that in addition to the primary use of test-mass charging monitoring, particle detectors on board space interferometers will naturally provide SEP observations at different intervals in heliolongitude and distances from Earth for space weather applications. PACS Number(s): 96.50.sb, 96.50.sh, 96.50.Vg, 94.05.Sd, 04.80.Nn, 95.55.Ym 1341006-1 Int. J. Mod. Phys. D 2013.22. Downloaded from www.worldscientific.com by QUEEN'S UNIVERSITY on 02/04/15. For personal use only. 1341006-2 Int. J. Mod. Phys. D 2013.22. Downloaded from www.worldscientific.com by QUEEN'S UNIVERSITY on 02/04/15. For personal use only.

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Section: Introductionmentioning

confidence: 77%

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Grimani

2013

Int. J. Mod. Phys. D

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“…Neither electron nor heavy-ion monitoring will be carried out on LISA-PF. The possibility of modifying the LISA-PF radiation monitors for LISA in order to include solar electron detection for SEP event forecasting was presented in [15].…”

Section: Radiation Detector On Board Lisa-pfmentioning

confidence: 99%

“…Solar and galactic particles with energies greater than 100 MeV/n penetrate the spacecraft charging the test masses [12][13][14]. This process constitutes one of the most important sources of noise for the experiment in the low-frequency range (see for example [15]).…”

Section: Introductionmentioning

confidence: 99%

On the role of radiation monitors on board LISA Pathfinder and future space interferometers

Grimani

Boatella

Chmeissani

et al. 2012

Class. Quantum Grav.

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LISA (Laser Interferometer Space Antenna) and its precursor mission LISA Pathfinder (LISA-PF) will carry particle monitors for noise diagnostics. It was proposed to build and place radiation detectors on board the ASTROD missions as well. We present here a study of the solar energetic particle (SEP) events that the LISA-PF radiation monitors are able to detect above the galactic cosmic-ray (GCR) background predicted at the time of the mission data taking in 2015. In order to optimize the correlation between radiation monitor measurements and gravitational sensor test-mass charging, the energy threshold for particles traversing both detectors should be approximately the same. In LISA-PF, the radiation monitor particle energy cut-off was conservatively set at 75 MeV per nucleon (MeV/n) for protons and ion normal incidence, while the minimum energy of the same particles reaching the test masses is 100 MeV/n. We find that SEP events detectable on LISA-PF are characterized by peak fluxes and fluences at energies >75 MeV/n larger than about 45%, on average, with respect to those at energies >100 MeV/n. We conclude that for an accurate correlation between radiation monitor count rates and test-mass charging, it is mandatory to benefit from absolute flux measurements of both galactic and high-energy solar particles provided by experiments carrying magnetic spectrometers in space at the time of LISA-PF (PAMELA, AMS). On the other hand, the role of the radiation detectors on board LISA-PF is crucial allowing for SEP event onset and dynamics monitoring.

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“…Ions with energies larger than 100 MeV(/n) penetrate the spacecraft and, therefore, particle detector observations will help to estimate the proof mass charging [20,21]. In particular, LISA simulations indicate that solar events with fluences larger than 10 7 protons/cm 2 overcome the whole mission noise budget in the low frequency range in a few tens of minutes ( [22] and references therein).…”

Section: Solar Physics Using Radiation Monitorsmentioning

confidence: 99%

“…Each event lasts a few days. It was evaluated if it was worthwhile to modify the LISA-PF radiation monitors to add SEP forecasting capabilities to LISA [21]. For the ASTROD I mission the test mass charging studies were reported in [23][24] for both galactic cosmic-ray and solar energetic particles.…”

Section: Solar Physics Using Radiation Monitorsmentioning

confidence: 99%

Astrodynamical Space Test of Relativity using Optical Devices I (ASTROD I)—a class-M fundamental physics mission proposal for cosmic vision 2015–2025: 2010 Update

et al. 2012

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ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test General Relativity with an improvement in sensitivity of over 3 orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals.For this mission, accurate pulse timing with an ultra-stable clock, and a drag-free spacecraft with reliable inertial sensor are required. T2L2 has demonstrated the required accurate pulse timing; rubidium clock on board Galileo has mostly demonstrated the required clock stability; the accelerometer on board GOCE has paved the way for achieving the reliable inertial sensor; the demonstration of LISA Pathfinder will provide an excellent platform for the implementation of the ASTROD I drag-free spacecraft. These European activities comprise the pillars for building up the mission and make the technologies needed ready. A second mission, ASTROD or ASTROD-GW (depending on the results of ASTROD I), is envisaged as a three-spacecraft mission which, in the case of ASTROD, would test General Relativity to one part per billion, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 parts per million, and probe gravitational waves at frequencies below the LISA bandwidth, or in the case of ASTROD-GW, would be dedicated to probe gravitational waves at frequencies below the LISA bandwidth to 100 nHz and to detect solar g-mode oscillations. In the third phase (Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD bandwidth. This paper on ASTROD I is based on our 2010 proposal submitted for the ESA call for class-M mission proposals, and is a sequel and an update to our previous paper (Appouchaux et al., Exp Astron 23:491–527, 2009; designated as Paper I) which was based on our last proposal submitted for the 2007 ESA call. In this paper, we present our orbit selection with one Venus swing-by together with orbit simulation. In Paper I, our orbit choice is with two Venus swing-bys. The present choice takes shorter time (about 250 days) to reach the opposite side of the Sun. We also present a preliminary design of the optical bench, and elaborate on the solar physics goals with the radiation monitor payload. We discuss telescope size, trade-offs of drag-free sensitivi...

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Short-term forecasting of solar energetic ions on board LISA

Cited by 6 publications

References 9 publications

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

On the role of radiation monitors on board LISA Pathfinder and future space interferometers

Astrodynamical Space Test of Relativity using Optical Devices I (ASTROD I)—a class-M fundamental physics mission proposal for cosmic vision 2015–2025: 2010 Update

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