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Detection and Measurement of Micrometeoroids with LISA Pathfinder

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Detection and Measurement of Micrometeoroids with LISA Pathfinder A&A 586, A107 (2016) Astronomy DOI: 10.1051/0004-6361/201527658 & c ESO 2016 Astrophysics Detection and measurement of micrometeoroids with LISA Pathfinder J. I. Thorpe1, C. Parvini1,2, and J. M. Trigo-Rodríguez3 1 Gravitational Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA e-mail: [email protected] 2 Department of Aerospace Engineering, The George Washington University, Washington, DC 20052, USA 3 Meteorites, Minor Bodies and Planetary Sciences Group, Institute of Space Sciences (CSIC-IEEC), Campus UAB Bellaterra, Carrer de Can Magrans, s/n 08193 Cerdanyola del Vallés Barcelona, Spain Received 28 October 2015 / Accepted 23 December 2015 ABSTRACT The Solar System contains a population of dust and small particles originating from asteroids, comets, and other bodies. These par- ticles have been studied using a number of techniques ranging from in-situ satellite detectors to analysis of lunar microcraters to ground-based observations of zodiacal light. In this paper, we describe an approach for using the LISA Pathfinder (LPF) mission as an instrument to detect and characterize the dynamics of dust particles in the vicinity of Earth-Sun L1. Launched on Dec. 3rd, 2015, LPF is a dedicated technology demonstrator mission that will validate several key technologies for a future space-based gravitational-wave observatory. The primary science instrument aboard LPF is a precision accelerometer which we show will be capable of sensing discrete momentum impulses as small as 4 × 10−8 N s. We then estimate the rate of such impulses resulting from impacts of microme- teoroids based on standard models of the micrometeoroid environment in the inner solar system. We find that LPF may detect dozens to hundreds of individual events corresponding to impacts of particles with masses >10−9 g during LPF’s roughly six-month science operations phase in a 5 × 105 km by 8 × 105 km Lissajous orbit around L1. In addition, we estimate the ability of LPF to charac- terize individual impacts by measuring quantities such as total momentum transferred, direction of impact, and location of impact on the spacecraft. Information on flux and direction provided by LPF may provide insight as to the nature and origin of the individ- ual impact and help constrain models of the interplanetary dust complex in general. Additionally, this direct in situ measurement of micrometeoroid impacts will be valuable to designers of future spacecraft targeting the environment around L1. Key words. meteorites, meteors, meteoroids – instrumentation: miscellaneous 1. Introduction Lissajous orbit around the first Sun-Earth (L1) lagrange point. LPF was launched on December 3rd, 2015 and will begin sci- Our current understanding of the interplanetary dust complex ence operations in early 2016 and continue for approximately six is informed by a number of measurement techniques including months with a possible extension of an additional six months. In photographic and visual meteors (Halliday et al. 1984; Hawkes this paper, we outline an approach for using LPF as an instru- 2007; Trigo-Rodriguez et al. 2008), radio meteors, atmospheric ment to detect and characterize interplanetary dust in the vicin- collections (Flynn 1994), observation of zodiacal light in thermal ity of L1. This technique does not require any modification to (Krick et al. 2012) and visual (Levasseur-Regourd & Dumont the hardware or operations of LPF and may provide an impor- 1980) wavelengths, in-situ penetration and ionization detectors tant new source of information to constrain models of the dust (Weidenschilling 1978; Zhang & Kessler 1995), and analysis complex. of microcraters in lunar samples (Allison & McDonnell 1982). The outline of the paper is as follows. In Sect. 2 we describe Additionally, NASA’s Stardust mission (Hörz et al. 2006)and the working principle of the LPF instrument and its application ESA’s Rosetta mission (Rotundi et al. 2015)havemadein-situ as a dust detection instrument. In Sect. 3 we make a simple es- measurements of the dust environments near the comets Wild 2 timate for the detection threshold of LPF as a function of trans- / and 67 Churyumov-Gerasimenko respectively. The combined ferred momentum using a simplified 1D model. In Sect. 4 we picture from all of these techniques, each with varying ability estimate the rates of events above this threshold and the total to detect and characterize various sub-populations of the dust number of likely events during the LPF mission. In Sect. 5 we complex, is used to constrain theoretical models that account for estimate the precision with which LPF will measure parameters the sources, sinks, and dynamics of the dust complex. of individual impacts such as momentum transferred and direc- The LISA Pathfinder (LPF) mission (Armano et al. 2015), tion of impact. In Sect. 6, we summarize our results and outline is a technology demonstration mission dedicated to validating likely avenues for refining the estimates made here. several key technologies for a future space-based observatory (Bender & Danzmann 1998; Jennrich 2011) of astrophysical gravitational waves (Einstein 1918; Bondi et al. 1959). Led by 2. Overview of technique the European Space Agency with contributions from NASA and a number of European research institutions, LPF consists of a Inside the LPF are two inertial sensor units each containing a single sciencecraft operating in a 5 × 105 km by 8 × 105 km test mass comprised of a 46 mm cube of Au-Pt alloy with a mass Article published by EDP Sciences A107, page 1 of 6 A&A 586, A107 (2016) 10-10 of 1.96 kg. During launch and cruise, these test masses are me- Thruster Inertial Sensor chanically supported by a lock mechanism, which is retracted 2 Total m Hz prior to beginning science operations leaving the test masses 2 4 s -12 freely-falling inside the inertial sensors with no mechanical con- kg 10 tacts. Each inertial sensor unit measures the position and attitude of its respective test mass relative to the LPF spacecraft in all six rigid-body kinematic degrees-of-freedom (DoFs) using a capaci- 10-14 tive sensing system. The inertial sensor unit can apply forces and torques to the test mass via electrostatic actuation. Additional in- formation is provided by a laser interferometer that measures a 10-16 three of DoFs (position, tip, and tilt) with higher precision and a star tracker which measures the three angular DoFs of the space- Equivalent Force Noise craft relative to a background inertial reference frame. A control 10-18 system converts the position and attitude measurements from the 10-4 10-3 10-2 10-1 100 two inertial sensors, the interferometer, and the star tracker into Fourier Frequency [ Hz] force and torque commands that are applied to the test masses Fig. 1. Power spectral density of equivalent spacecraft force noise in a and the spacecraft, the latter being actuated using a microthruster simplified one-dimensional model of LPF. system. The main purpose of the control system is to reduce exter- ≤ ≤ nal force disturbances on the test masses; low-disturbance ref- noise on the spacecraft in the measurement band 0.1mHz f erence masses are a key technology for LISA-like instruments. 100 mHz. The first is the noise of the microthruster system itself, A byproduct of this effort is an exquisite measurement of exter- which is characterized by a flat power spectral density with a nal force disturbances on the LPF spacecraft either through the level of −16 2 residual motion between the spacecraft and the test masses or in S th ≈ 10 N /Hz, (3) the applied control forces and torques. One such source of ex- ternal force disturbance is an impulse generated by an impact of The thruster noise dominates at low frequencies but is eclipsed a micrometeoroid or dust particle. In the following sections, we above a few mHz by the equivalent force noise of the inertial estimate the detection threshold and rate for such impact events. sensor. The inertial sensor noise is characterized by a flat dis- placement amplitude spectral density at a level of ∼2nm/Hz1/2. This can be converted to an equivalent force noise on the space- 3. Detection threshold craft by multiplying by the spacecraft mass (M = 422 kg) and taking two time derivatives. The resulting power spectral density The momentum transferred to the LPF spacecraft by an indi- of this equivalent spacecraft force noise from the inertial sensor vidual micrometeoroid impact will combine with stochastic dis- is given by turbances on the spacecraft from a number of sources such as −9 1/2 2 2 Solar radiation pressure, outgassing, and noise from the mi- S is ≈ (2 × 10 m/Hz ) · M · (2π f ) crothruster system. The measured momentum transfer will also −9 4 2 5 be effected by noise in the position sensing system and force = 1.1 × 10 · f N /Hz . (4) disturbances on the test masses. To simplify our estimate of the The individual and combined components of the spacecraft threshold at which LPF can detect an individual impact, we con- equivalent force noise are shown in Fig. 1. sider a simplified one-dimensional model in a linear DoF. We An impact by a micrometeoroid is modeled as an impulsive adopt the maximum-likelihood formalism, where the signal-to- τ P / force occurring at time and imparting a total momentum over noise ratio (S N) of an event is defined using a noise-weighted a characteristic timescale Δ. This can be written in the time and inner-product: frequency domains respectively as: ρ2 = F|F, (1) = P Θ − − Θ − − Δ F(t) Δ [ (t τ) (t τ )] , (5) where ρ is the S/N, F is the “waveform” of the force on the −2πif(τ+Δ/2) spacecraft resulting from the impact and ...| ..
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