## 2 Analysis of Astrophysical Data  
Drawing on astrophysical research [10; 11; 12; 13; 14; 15; 16; 17; 18; 19; 20; 21; 22; 23], we briefly delve into the physical properties of matter in near-Earth space that are required, analyzing the efficiency of the proposed scheme. The primary constituents of interplanetary matter we focus on are the solar wind, high-energy charged particles, interplanetary dust, and neutral gas [19; 20; 21; 22]. Solar wind mainly comprises of hydrogen plasma, with a minute portion of helium ions, generated from the transfer processes within the Sun's corona. Direct observations [10; 11; 12; 13; 14; 16; 23] suggest the formation of non-stationary, spherically asymmetric flows that vary significantly over time depending on the solar corona's state. Plasma expulsion creates non-stationary shockwaves within the interplanetary space close to the Sun, exhibiting sudden changes in velocity, density, and temperature when faster flows overtake slower ones. As these waves move away from the Sun, they interact, resulting in a quasi-stationary plasma flow at a distance of about one Astronomical Unit (\(A.U.\)) directly in near-Earth space. This flow constantly contains a relatively slower part of the solar wind with typical speeds of \(300\div 500\) km/s and a density of \(10\div 15\) cm\({}^{-3}\)[19; 23], originating from the gas-dynamic expansion of the solar corona's \"quiet\" portion (the so-called slow flow). The  
Figure 1: Spacecraft diagram: 1—interplanetary dust; 2—particle trap; 3—the spacecraft’s movement direction; 4—discharge chamber; 5—ship; 6—solar panel; 7—plasma flow creating the ship’s thrust [9]. quasi-stationary flow (the so-called fast flow), with speeds of \(700\div 1000\) km/s and a density of \(3\div 4\) cm\({}^{-3}\), comprises particles emanating directly from the Sun's surface [16; 19; 23]. This phenomenon appears within several months and repeats every 27 days. Another component is the relativistic flow of protons generated during solar flares, but this is typically short-lived and sparse; thus, its contribution is often disregarded [19; 23]. As a result, the quasi-stationary plasma flow's average speed is \(v_{sw}=400\div 500\) km/s with a density range of \(10\leq n_{sw}\leq 20\) cm\({}^{-3}\), as observed in Earth's orbit [10; 19; 23]. As was shown in [10; 23], both the pressure gradient and the Sun's gravitational force can be ignored at a distance of around 1 \(A.U.\) This implies that for distances \(r>1\)\(A.U.\), the wind speed can be considered steady, and the flow's density declines with the distance as a function, \(r^{-2}\), whereas at a distance of \(r=2\)\(A.U.\), the density would fall within the \(2\leq n_{sw}\leq 5\) cm\({}^{-3}\) range. Therefore, this \(n_{sw}\) value can be utilized for approximate calculations within a distance range of \(1\leq r\leq 2\)\(A.U.\) Clearly, if \(r<1\)\(A.U.\), this value would increase as we move closer to the Sun. Now, we shall move on to discussing the component composition of cosmic dust. According to [14; 15; 17; 19], interplanetary dust comprises three main chemical elements: magnesium (Mg), silicon (Si), and iron (Fe). The present elements are included in approximately equal proportions, and silicon has the highest ionization potential, \(\epsilon_{i}=8.15\) eV [14; 19]; this value will be used in subsequent estimations. One can expect that these components create the main part of the thrust since they have the largest atom masses and the highest percentages in the compounds of interplanetary dust. To simplify the present rude calculations, instead of all dust components, we introduce a \"medial\" dust particle with mass \(\mu_{\Sigma}=\left(\mu_{Mg}+\mu_{Si}+\mu_{Fe}\right)/3\approx 60\times 10^{-27}\) kg, where \(\mu_{Mg}\), \(\mu_{Si}\), and \(\mu_{Fe}\) are the molecular weights of magnesium, silicon, and iron, respectively. Proceeding from this point, we can approximate the density of dust particles by estimating the annual influx of dust from the zodiacal cloud into Earth's atmosphere as it orbits the Sun.