Magnetic sail

A plasma consists exclusively of charged particles that can interact with a magnetic or electric field. It does not include neutral particles, such as neutrons. atoms or molecules.The plasma mass density ρ used in magnetohydrodynamic models only require a weighted average mass density of charged particles that includes neutrons in the ion, while kinematic models use the values for each specific ion type and in some cases the parameters for electrons as well as described below, a paragraph that can be skipped without loss of meaning.

The velocity distribution of ions and electrons is another important parameter but often analyses use only the average velocity for the aggregate of particles in a plasma wind for a particular plasma environment (pe) is ${\displaystyle v_{pe}}$. The apparent wind velocity ${\displaystyle u_{sc}}$ as seen by a spacecraft traveling at velocity ${\displaystyle v_{sc}}$ (positive meaning acceleration in the same direction as the wind and negative meaning deceleration opposite the wind direction) for a particular plasma environment (pe) is ${\displaystyle u_{sc}=v_{pe}-v_{sc}}$.

A plasma environment has fundamental parameters, and if a cited reference uses cgs units these should be converted to SI units as defined in the NRL plasma formulary,[25] which this article uses as a reference for plasma parameter units not defined in SI units. The major parameters for plasma mass density are: the number of ions of type ${\displaystyle i}$ per unit volume ${\displaystyle n_{i}}$ the mass of each ion type accounting for isotopes ${\displaystyle m_{i}}$ and the number of electrons ${\displaystyle n_{e}}$ per unit volume each with electron mass ${\displaystyle m_{e}}$.[26] An average plasma mass density per unit volume for charged particles in a plasma environment ${\displaystyle pe}$ (${\displaystyle sw}$ for stellar wind, ${\displaystyle pi}$ for planetary ionosphere, ${\displaystyle im}$ for interstellar medium) is expressed in equation form to unambiguously define the meaning of an averaged mass density for charged particles ${\displaystyle \textstyle \rho _{pe}=n_{e}m_{e}+\sum _{i}n_{i}m_{i}}$. In SI units per unit volume is cubic metre (m^-3), mass is kilogram (kg), and mass density is kilogram per cubic metre (kg/m³).

Many designs, analyses, simulations and experiments focus on using a magnetic sail in the solar wind plasma to accelerate a spacecraft away from the Sun.[2] Near the Earth's orbit at 1 AU the plasma flows at velocity ${\displaystyle v_{sw}}$ dynamically ranges from 250 to 750 km/s (typically 500), with a density ranging from 3 to 10 particles per cubic centimeter (typically 6) as reported by the NOAA real-time solar wind tracking web site[27] Assuming that 8% of the solar wind is helium and the remainder hydrogen, the average solar wind plasma mass density at 1 AU is ${\displaystyle 4\times 10^{-21}<\rho _{sw}(1)<10^{-20}}$ kg/m³ (typically 10⁻²⁰ kg/m³).[28]

The average plasma mass density of ions ${\displaystyle \rho _{sw}}$ decreases according to an Inverse-square law with the distance from the Sun, ${\displaystyle a_{\odot }}$. In order to substitute this into another equation the curve fit formula for values near the Sun with the dimension for ${\displaystyle a_{\odot }}$ being astronomical units (AU) is ${\displaystyle \rho _{sw}(a_{\odot })=\rho _{sw}(1)/a_{\odot }^{2}}$.[29] ^{: Fig 5} The velocity for values near the Sun is nearly constant, falling off slowly after 1 AU[29]^{: Fig 5} and then rapidly decreasing at heliopause.

A spacecraft accelerated to very high velocities by other means, such as a fusion rocket or laser pushed lightsail, can decelerate even from relativistic velocities without onboard propellant by using a magnetic sail to create thrust (drag) against the interstellar medium plasma environment. As shown in the section on Magsail kinematic model (MKM), feasible uses of this involve maximum velocities below 10% c, taking decades to decelerate, for total travel times on the order of a century as described in the magsail specific designs section.

Only the magsail references consider deceleration in the ISM on approach to Alpha (${\displaystyle \alpha }$) Centauri. As shown in the figure, the local bubble and G-cloud are between the Solar System that is moving at velocity ${\displaystyle v_{sun}}$and the local cloud is moving at velocity ${\displaystyle v_{L|C}}$. Alpha Estimates of the number of protons range between 0.005 and 0.5 cm⁻³ resulting in a plasma mass density ${\displaystyle 9\times 10^{-24}<\rho _{im}<3\times 10^{-22}}$ kg/m³ , which covers the range used by references in the magsail specific designs section. As summarized in the magsail specific design section, Gros cited references indicating that regions of the G-clouds may be colder and have a low ion density. A typical value assumed for approach to Alpha Centauri is a proton number density ${\displaystyle n_{i}}$of 0.1 protons per cm³ [30] corresponding to ${\displaystyle \rho _{im}\approx 10^{-22}}$ kg/m³.

The spacecraft velocity ${\displaystyle v_{sc}}$ is much greater than the ISM velocity at the beginning of a deceleration maneuver so the apparent plasma wind velocity from the spacecraft's viewpoint s approximately ${\displaystyle u_{im}\approx -v_{sc}}$.

Radio emissions of cyclotron radiation due to interaction of charged particles in the interstellar medium as they spiral around the magnetic field lines of a magnetic sail would have a frequency of approximately ${\displaystyle 120\,v_{sc}/c}$ kHz.[31] The Earth's ionosphere would prevent detection on the surface, but a space-based antenna could detect such emissions up to several thousands of light years away. Detection of such radiation could indicate activity of advanced extraterrestrial civilizations.

A spacecraft approaching a planet with a significant upper atmosphere such as Saturn or Neptune could use a magnetic sail to decelerate by ionizing neutral atoms such that it behaves as a low beta plasma.[18][20] The plasma mass density in a planetary ionosphere (pi) ${\displaystyle \rho _{pi}}$ is comprised of multiple ion types and varies by altitude. The spacecraft velocity ${\displaystyle v_{sc}}$ is much greater than the planetary ionosphere velocity in a deceleration maneuver so the apparent plasma wind velocity is approximately ${\displaystyle u_{pi}\approx -v_{sc}}$ at the beginning of a deceleration maneuver.

Inside or near a planetary magnetosphere, a magnetic sail can thrust against or be attracted to a planet's magnetic field created by a dynamo, especially in an orbit that passes over the planet's magnetic poles.[5] When the magnetic sail and planet's magnetic field are in opposite directions an attractive force occurs and when the fields are in the same direction a repulsive force occurs, which is not stable and means to prevent the sail from flipping over is necessary.

The thrust that a magnetic sail delivers within a magnetosphere decreases with the fourth power of its distance from the planet's internal magnetic field. When close to a planet with a strong magnetosphere such as Earth or a gas giant, the magnetic sail could generate more thrust by interacting with the magnetosphere instead of the solar wind. When operating near a planetary or stellar magnetosphere the effect of that magnetic field must be considered if it is on the same order as the gravitational field.

By varying the magnetic sail's field strength and orientation a "perigee kick" can be achieved raising the altitude of the orbit's apogee higher and higher, until the magnetic sail is able to leave the planetary magnetosphere and catch the solar wind. The same process in reverse can be used to lower or circularize the apogee of a magsail's orbit when it arrives at a destination planet with a magnetic field.

In theory, it is possible for a magnetic sail to launch directly from the surface of a planet near one of its magnetic poles, repelling itself from the planet's magnetic field. However, this requires the magnetic sail to be maintained in an "unstable" orientation. Furthermore, the magnetic sail must have extraordinarily strong magnetic fields for a launch from Earth, requiring superconductors supporting 80 times the current density of the best known high-temperature superconductors as of 1991.[5]

In 2022 a spaceflight trial dubbed Jupiter Observing Velocity Experiment (JOVE) proposed using a plasma magnet to decelerate against the magnetosphere of Jupiter.[17]

An ion or electron with charge q in a plasma moving at velocity v in a magnetic field B and electric field E is treated as an idealized point charge in the Lorentz force (N) ${\displaystyle \mathbf {F} =q\,\mathbf {E} +q\,\mathbf {v} \times \mathbf {B} }$. This means that the force on an ion or electron is proportional to the product of their charge q and velocity component ${\displaystyle v}$ perpendicular to the magnetic field flux density B, in SI units as teslas (T). A magnetic sail design introduces a magnetic field into a plasma flow which under certain conditions deflects the electrons and ions from their original trajectory with the particle's momentum transferred to the sail and hence the spacecraft thereby creating thrust.[2] An electric sail uses an electric field E that under certain conditions interact with charged particles to create thrust.

Artificial magnetospheric model

The characteristics of the Earth's magnetosphere have been widely studied as a basis for magnetic sails. The figure shows streamlines of charged particles from a plasma wind from the Sun (or a star) or an effective wind when decelerating in the ISM flowing from left to right. A source attached to a spacecraft generates a magnetic field. Under certain conditions at the boundary where magnetic pressure equals the plasma wind kinetic pressure an artificial magnetopause forms at a characteristic length ${\displaystyle L}$ from the field source. The ionized plasma wind particles create a current sheet, known as the Chapman–Ferraro current along the magnetopause, which compresses the magnetic field lines facing the oncoming plasma wind by a factor of 2 at magnetopause as shown in Figure 2a.[1] The magnetopause deflects charged particles, which affects their streamlines and increases the density at magnetopause. A magnetospheric bubble or cavity forms that has very low density downstream from the magnetopause. Upstream from the magnetopause a bow shock develops. Simulation results often show the particle density through use of color with an example shown in the figure according to the legend in the lower left. This figure uses aspects of the general structure from Figure 3[4] Figure 1[32] and Figure 2a,[1] and aspects of the plasma density from Figure 1,[33] and Figure 2.[34]

Magnetic sail designs operating in a plasma wind share a theoretical foundation based upon a magnetohydrodynamic (MHD) model, sometimes called a fluid model, from plasma physics for an artificially generated magnetosphere. Under certain conditions, the plasma wind and the magnetic sail are separated by a magnetopause that blocks the charged particles, which creates a drag force that transfers (at least some) momentum to the magnetic sail, which then applies thrust to the attached spacecraft.[35][36][1][32]

Artificial Magnetosphere Model of Basic Magnetic Sail

The figure depicts the MHD model.[1][2] Starting from the left a plasma wind in a plasma environment (e.g., stellar, ISM or an ionosphere) of effective velocity ${\textstyle v_{pe}}$ with density ${\textstyle \rho _{pe}}$ encounters a spacecraft with time-varying velocity ${\textstyle v_{sc}}$ that is positive if accelerating and negative if decelerating. The apparent plasma wind velocity from the spacecraft's viewpoint is ${\textstyle u_{pe}=v_{pe}-v_{sc}}$. The spacecraft and field source generate a magnetic field that creates a magnetospheric bubble extending out to a magnetopause preceded by a bow shock that deflects electrons and ions from the plasma wind At magnetopause the field source magnetic pressure equals the kinetic pressure of the plasma wind at a standoff shown at the bottom of the figure. The characteristic length ${\textstyle L}$ is that of a circular sail of effective blocking area ${\displaystyle S=\pi \,R_{mp}^{2}}$ where ${\displaystyle R_{mp}\approx L}$ is the effective magnetopause radius. Under certain conditions the plasma wind pushing on the artificial magnetosphere bow shock and magnetopause creates a force ${\textstyle F_{w}}$ on the magnetic field source that is physically attached to the spacecraft so that at least part of the force ${\textstyle F_{w}}$ causes a force ${\textstyle F_{sc}}$on the spacecraft, accelerating it when sailing downwind or decelerating when sailing into a headwind. Under certain conditions and in some designs, some of the plasma wind force may be lost as indicated by ${\textstyle F_{loss}}$ on the right side.

All magnetic sail designs assume a standoff between plasma wind pressure ${\displaystyle p_{w}}$ and magnetic pressure ${\textstyle p_{B}}$ of the same form with parameters specific to a plasma environment, differing only in a constant coefficient ${\displaystyle C_{SO}}$ as follows:

${\displaystyle p_{w}=\rho u^{2}=p_{B}={\frac {B_{mp}^{2}}{C_{SO}\mu _{0}}}}$

(MHD.1)

where ${\textstyle u}$ is the apparent wind velocity and ${\displaystyle \rho }$ is the plasma mass density for a specific plasma environment, ${\displaystyle B_{mp}}$ T the magnetic field strength at magnetopause, μ₀ is the vacuum permeability(N A^-2) and ${\textstyle C_{SO}}$ is a constant that differs by reference as follows for ${\textstyle C_{SO}=2}$ corresponding to ${\textstyle p_{w}}$modeled as dynamic pressure with no magnetic field compression,[32] ${\textstyle C_{SO}=1}$ for ${\textstyle p_{w}}$modeled as ram pressure (Pa) with no magnetic field compression[4][16] and ${\textstyle C_{SO}=1/2}$ for ${\textstyle p_{w}}$ modeled as ram pressure with magnetic field compression by a factor of 2[1] Equation MHD.1 can be solved to yield the required magnetic field ${\displaystyle B_{mp}}$ that satisfies the pressure balance at magnetopause standoff as:

$${\displaystyle B_{mp}=u{\sqrt {\rho \,\mu _{0}\,C_{SO}}}}$$

(MHD.2)

The solar wind plasma density ρ(${\displaystyle a_{\odot }}$) decreases in inverse proportion to the square of the distance ${\displaystyle a_{\odot }}$ from the Sun and hence from the above, ${\displaystyle B_{mp}}$ decreases in inverse proportion to ${\displaystyle a_{\odot }}$. Since magnetic field strength at radius ${\displaystyle r}$ is ${\displaystyle B\propto 1/r^{3}}$ this means that the magnetic sail magnetopause radius ${\textstyle R_{mp}}$ will increase with distance from the Sun, where the increased effective size of a sail adjusts for the reduced dynamic pressure of the solar wind.[16] Plasma mass density may also change in the ISM and in a planetary ionosphere. The force derived by a magnetic sail for a plasma environment is determined from MHD equations as reported by many researchers is:[2][1][16][35][32]

$${\displaystyle F_{w}=C_{d}\ \rho {\frac {u^{2}}{2}}S=C_{d}\ \rho {\frac {u^{2}}{2}}\pi L^{2}}$$

(MHD.3)

where ${\textstyle C_{d}}$ is a coefficient of drag determined by numerical analysis and/or simulation, ${\textstyle \rho u^{2}/2}$ is the dynamic wind pressure, and ${\displaystyle S=\pi R_{mp}^{2}}$ is the effective blocking area of the magnetic sail with magnetopause radius ${\textstyle R_{mp}\approx L}$. Note that this equation has the same form as the drag equation in fluid dynamics. ${\textstyle C_{d}}$ is a function of coil attack angle on thrust and steering angle. The power(W) of the plasma wind is the product of velocity and a constant force

$${\displaystyle P_{w}=u\,F_{w}=C_{d}\ \rho {\frac {u^{3}}{2}}\pi R_{mp}^{2}={\frac {C_{d}u\pi }{2\mu _{0}C_{SO}}}R_{mp}^{2}B_{mp}^{2}}$$

(MHD.4)

where equation MHD.2 was used to derive the right-side yielding the same result as equation (9).[16]

Through analysis, numerical calculation, simulation and experimentation an important condition for a magnetic sail to generate significant force is the MHD applicability test,[37] that states that the standoff distance ${\displaystyle L}$ must be significantly greater than the ion gyroradius, also called the Larmor radius[1] or cyclotron radius:

$${\displaystyle r_{g}={\frac {m_{i}v_{\perp }}{\mid q\mid B_{x}C_{Li}}}}$$

(MHD.5)

where ${\textstyle m_{i}}$ is the ion mass, ${\displaystyle v_{\perp }}$ is the velocity of a particle perpendicular to the magnetic field, ${\displaystyle |q|}$ is the elementary charge of the ion, ${\textstyle B_{x}}$ is the magnetic field strength at the point of reference ${\textstyle x}$ and ${\textstyle C_{Li}}$ is a constant that differs by source with ${\textstyle C_{Li}=1}$ [16] and ${\textstyle C_{Li}=2}$[1]. For example, from Equation (7) of [1] in the solar plasma wind with 5 ions/cm³ at 1 AU with ${\displaystyle m_{i}}$ the proton mass (kg) , ${\displaystyle v_{\perp }=v_{sw}}$ = 400 km/s, ${\displaystyle B_{x}=B_{mp}}$ = 36 nT with ${\displaystyle C_{SO}}$=0.5 at from equation MHD.2 at magnetopause and ${\textstyle C_{Li}}$=2 then ${\displaystyle r_{g}\approx }$ 72 km. The MHD applicability test is the ratio ${\textstyle r_{g}/L}$. The figure plots ${\displaystyle C_{d}}$ on the left axis and lost thrust on the right axis versus the ratio ${\textstyle r_{g}/L}$. When ${\displaystyle r_{g}/L<1}$, ${\displaystyle C_{d}=3.6}$ is maximum, at ${\textstyle r_{g}/L\approx 1}$, ${\textstyle C_{d}=2.7}$, a decrease of 25% from the maximum and at ${\textstyle r_{g}/L\approx 2}$, ${\textstyle C_{d}\approx 1.5}$, a 45% decrease. As ${\displaystyle r_{g}/L}$ increases beyond one, ${\displaystyle C_{d}}$ decreases meaning less thrust from the plasma wind transfers to the spacecraft and is instead lost to the plasma wind. In 2004, Fujita[38][1] published numerical analysis using a hybrid PIC simulation using a magnetic dipole model that treated electrons as a fluid and a kinematic model for ions to estimate the coefficient of drag ${\displaystyle C_{d}}$ for a magnetic sail operating in the radial orientation resulting in the following approximate formula:

$${\displaystyle C_{d}(r_{g}/L)={\begin{cases}3.6\,e^{-0.28(r_{g}/L)^{2}},&{\text{for }}r_{g}/L<1\\{\frac {3.4}{r_{g}/L}}e^{-0.22(L/r_{g})^{2}},&{\text{for }}r_{g}/L\geq 1\end{cases}}}$$

(MHD.6)

The lost thrust is ${\displaystyle T_{loss}=(1-C_{d}(r_{g}/L))/3.6}$.

Coil magnetic field orientation and forces

In 2005 Nishida and others published results from numerical analysis of an MHD model for interaction of the solar wind with a magnetic field of current flowing in a coil that momentum is indeed transferred to the magnetic field produced by field source and hence to the spacecraft.[39] Thrust force derives from the momentum change of the solar wind, pressure by the solar wind on the magnetopause from equation MHD.1 and Lorentz force from currents induced in the magnetosphere interacting with the field source. The results quantified the coefficient of drag, steering (i.e., thrust direction) angle with the solar wind, and torque generated as a function of attack angle (i.e., orientation) The figure illustrates how the attack (or coil tilt) angle ${\displaystyle \alpha _{t}}$ orientation of the coil creates a steering angle for the thrust vector and also torque imparted to the coil. Also shown is the vector for the interplanetary magnetic field (IMF), which at 1 AU varies with waves and other disturbances in the solar wind, known as space weather, and can significantly increase the thrust of a magnetic sail.[40]

For a coil with radial orientation (like a Frisbee) the attack angle ${\displaystyle \alpha _{t}}$= 0° and with axial orientation (like a parachute) ${\displaystyle \alpha _{t}}$=90°. The Nishida 2005 results[39] reported a coefficient of drag ${\displaystyle C_{d}}$ that increased non-linearly with attack angle from a minimum of 3.6 at ${\displaystyle \alpha _{t}}$=0 to a maximum of 5 at ${\displaystyle \alpha _{t}}$=90°. The steering angle of the thrust vector is substantially less than the attack angle deviation from 45° due to the interaction of the magnetic field with the solar wind. Torque increases from ${\displaystyle \alpha _{t}}$= 0° from zero at to a maximum at ${\displaystyle \alpha _{t}}$=45° and then decreases to zero at ${\displaystyle \alpha _{t}}$=90°. A number of magnetic sail design and other papers cite these results. In 2012 Kajimura reported simulation results[41] that covered two cases where MHD applicability occurs with ${\displaystyle r_{g}/L}$=1.125 and where a kinematic model is applicable ${\displaystyle r_{g}/L}$=0.125 to compute a coefficient of drag ${\displaystyle C_{d}}$ and steering angle. As shown in Figure 4 of that paper when MHD applicability occurs the results are similar in form to Nishida 2005[39] where the largest ${\displaystyle C_{d}}$ occurs with the coil in an axial orientation. However, when the kinematic model applies, the largest ${\displaystyle C_{d}}$ occurs with the coil in an radial orientation. The steering angle is positive when MHD is applicable and negative when a kinematic model applies. The 2012 Nishida and Funaki published simulation results [42] for a coefficient of drag ${\displaystyle C_{D}}$, coefficient of lift ${\displaystyle C_{L}}$ and a coefficient of moment ${\displaystyle C_{M}}$ for a coil radius of ${\displaystyle R_{c}}$=100 km and magnetopause radius ${\displaystyle R_{mp}}$=500 km at 1 AU.

In a design, either the magnetic field source strength or the magnetopause radius ${\displaystyle R_{mp}\approx L}$ the characteristic length must be chosen. A good approximation[36][32] for a magnetic field falloff rate ${\displaystyle f_{o},1\leq f_{o}\leq 3}$ for a distance ${\textstyle R_{0}\leq r\leq R_{mp}}$ from the field source to magnetopause starts with the equation:

${\displaystyle B(r)\approx B(R_{0}){\biggl (}{\frac {R_{0}}{r}}{\biggr )}^{f_{o}}}$

(MFM.1)

where ${\displaystyle B(R_{0})}$ is the magnetic field at a radius ${\displaystyle R_{0}}$ near the field source that falls off near the source as ${\displaystyle 1/r^{3}}$ as follows:

${\displaystyle B(R_{0})\approx C_{0}{\frac {\mu _{0}\,\mathbf {m} }{4\,\pi \,R_{0}^{3}}}}$

(MFM.2)

where ${\displaystyle C_{0}}$ is a constant multiplying the magnetic moment (A m²) ${\displaystyle \mathbf {m} }$ to make ${\displaystyle B(r)}$ match a target value at ${\textstyle r>>R_{0}}$. When far from the field source, a magnetic dipole is a good approximation and choosing the above value of ${\displaystyle B(R_{0})}$ with ${\displaystyle C_{0}}$ =2 near the field source was used by Andrews and Zubrin.[4]

The Amperian loop model for the magnetic moment is ${\displaystyle \mathbf {m} =I_{c}S}$, where ${\displaystyle I_{c}}$ is the current in Amperes (A) and ${\displaystyle S=\pi \,R_{c}^{2}}$ is the surface area for a coil (loop) of radius ${\displaystyle R_{c}}$. Assuming that ${\displaystyle R_{0}\approx R_{c}}$ and substituting the expression for the magnetic moment ${\displaystyle \mathbf {m} }$ into equation MFM.2 yields the following:

${\displaystyle I_{c}={\frac {4}{C_{0}\mu _{0}}}B(R_{c})\,R_{c}}$

(MFM.3)

When the magnetic field flux density ${\displaystyle B(R_{0})}$ is specified, substituting ${\displaystyle B_{mp}}$ from the pressure balance analysis from equation MHD.2 into the above and solving for ${\textstyle R_{mp}}$ yields the following:

${\displaystyle L\approx R_{mp}\approx R_{0}{\biggl (}{\frac {B(R_{0})}{B_{mp}}}{\biggr )}^{1/f_{o}}}$

(MFM.4)

This is the expression for ${\displaystyle L}$ when ${\displaystyle f_{o}=3}$ with ${\displaystyle C_{SO}=1/2}$[1]^{: Eq (4)} and ${\displaystyle C_{SO}=2}$[32]^{: Eq (4)} and is the same form as the magnetopause distance of the Earth. Equation MFM.4 shows directly how a decreased falloff rate ${\displaystyle f_{o}}$ dramatically increases the effective sail area ${\displaystyle S=\pi R_{mp}^{2}}$ for a given field source magnetic moment ${\displaystyle \mathbf {m} }$ and ${\displaystyle B_{mp}}$ determined from the pressure balance equation MHD.1. Substituting this into equation MHD.3 yields the plasma wind force as a function of falloff rate ${\displaystyle f_{o}}$, plasma density ${\displaystyle \rho }$, coil radius ${\displaystyle R_{c}\approx R_{0}}$, coil current ${\displaystyle I_{c}}$ and plasma wind velocity ${\displaystyle u}$ as follows:

${\displaystyle F_{w}(f_{o})={\frac {C_{d}}{2}}\rho u^{2}\,\pi \,R_{0}^{2}\,{\biggl (}{\frac {B(R_{0})}{B_{mp}}}{\biggr )}^{2/f_{o}}={\frac {C_{d}}{2}}\rho u^{2}\,\pi \,R_{0}^{2}\,{\biggl (}{\frac {{\sqrt {\mu _{0}}}I_{c}C_{0}}{4R_{0}\,u{\sqrt {\rho \,C_{SO}}}}}{\biggr )}^{2/f_{o}}}$

(MFM.5)

using equation MFM.3 for ${\displaystyle B(R_{0})}$ and equation MHD.2 for ${\displaystyle B_{mp}}$. This is the same expression as equation (10b) when ${\displaystyle f_{o}=3}$ and ${\displaystyle C_{SO}=1/2}$[2] and[7]^{: Eq (108)} and the right hand side from equation (20) specifically applied to M2P2[32] with other numerical coefficients grouped into the ${\displaystyle C_{d}}$ term. Note that force increases as falloff rate decreases. For the solar wind case, substituting MHD.2 into MFM.5 and using the function for the solar wind plasma mass density ${\displaystyle \rho _{sw}(a_{\odot })=\rho _{sw}(1)/a_{\odot }^{2}}$, with ${\displaystyle a_{\odot }}$ the distance from the sun in Astronomical units (AU) results in the following expression

${\displaystyle F_{w}(f_{o},a_{\odot })=C_{f_{o}}\,(\rho _{sw}(a_{\odot })\,u^{2}))^{1-1/f_{o}}\,R_{0}^{2}\,S}$

(MFM.6)

where ${\displaystyle C_{f_{o}}={\frac {C_{d}}{2}}{\biggl (}{\frac {B(R_{0})^{2}}{\mu _{0}C_{SO}}}{\biggr )}^{1/f_{o}},{\mathsf {and}}\,S=\pi \,R_{mp}^{2}}$, the effective sail blocking area.

This equation explicitly shows the relationship upon plasma mass density ${\displaystyle \rho (a_{\odot })}$ as a function of distance from the Sun ${\displaystyle a_{\odot }}$. For the case ${\displaystyle f_{o}}$=1 the expansion of the magnetopause radius ${\displaystyle R_{mp}}$ exactly matches the decreasing value of ρ exactly as the distance from the Sun ${\displaystyle a_{\odot }}$ increases, resulting in constant force and hence constant acceleration inside the heliosphere.[16] Note that ${\displaystyle C_{f_{o}}}$ includes the term ${\displaystyle B(R_{0})^{2/f_{o}}}$, which means that as ${\displaystyle f_{o}}$ increases that the magnetic field near the field source ${\displaystyle B(R_{0})}$ must increase to maintain the same force for a smaller value of ${\displaystyle f_{o}}$. The example in the overview section set ${\displaystyle C_{f_{o}}}$=1, ${\displaystyle u}$=1, ${\displaystyle R_{0}}$=1, and ${\displaystyle S}$=1 so that the force at ${\displaystyle a_{\odot }}$=1 was equal for all values of ${\displaystyle f_{o}}$.

When the MHD applicability test of ${\textstyle r_{g}/L}$ <1 then a kinematic simulation model more accurately predicts force transferred from the plasma wind to the spacecraft. In this case the effective sail blocking area ${\displaystyle A_{e}}$ < ${\displaystyle S=\pi L^{2}}$.

Magnetic dipole force: MHD and kinematic models

The left axis of the figure is for plots of magnetic sail force versus characteristic length ${\displaystyle L}$. The solid black line plots the MHD model force ${\displaystyle F_{MHD}}$ from equation MHD.3. The green line shows the value of ion gyroradius ${\displaystyle r_{g}\approx }$ 72 km at 1 AU from equation MHD.5. The dashed blue line plots the hybrid MHD/kinematic model from equation MHD.6 from Fujita04.[38] The red dashed line plots a curve fit to simulation results from Ashida14.[24] Although a good fit for these parameters, the curve fit range of this model does not cover some relevant examples. Additional simulation results from Hajiwara15[43] are shown for the MHD and kinematic model as single data points as indicated in the legend. These models are all in close agreement. The kinematic models predict less force than predicted by the MHD model. In other words, the fraction ${\displaystyle T_{loss}}$ of thrust force predicted by the MHD model is lost when ${\displaystyle r_{g}/L<1}$ as plotted on the right axis. The solid blue and red lines show ${\displaystyle T_{loss}}$ for Fujita04[38] and Ashida18[24] respectively, indicating that operation with ${\displaystyle L}$ less than 10% of ${\displaystyle r_{g}}$ will have significant loss. Other factors in a specific magnetic sail design may offset this loss for values of ${\displaystyle L<r_{g}}$.

Important measures that determine the relative performance of different magnetic sail systems include: mass of the field source generator and its power and energy requirements; thrust achieved; thrust to weight ratio, any limitations and constraints, and propellant system exhausted, if any . Mass of the field source ${\displaystyle M_{fs}}$ in the Magsail design was relatively large and subsequent designs strove to reduce this measure. Total spacecraft mass is ${\displaystyle M_{sc}=M_{fs}+M_{p}}$, where ${\displaystyle M_{p}}$ is the payload mass. Power requirements are significant in some designs and add to field source mass. Thrust is the plasma wind force ${\displaystyle F_{w}}$ for a particular plasma environment with acceleration ${\displaystyle a=F_{w}/M_{sc}}$. The thrust to weight ratio ${\textstyle F_{w}/M_{sc}}$is also an important performance measure. Other limitations and constraints may be specific to a particular design. The M2P2 and MPS designs, as well as potentially the plasma magnet design, exhaust some plasma as part of inflating the magnetospheric bubble and these cases also have a specific impulse and effective exhaust velocity performance measure.

Andrews was working on use of a magnetic scoop to gather interstellar material as propellant for a nuclear electric ion drive spacecraft, allowing the craft to operate in a similar manner to a Bussard ramjet. Andrews asked Zubrin to help compute the magnetic scoop drag against the interplanetary medium, which turned out to be much greater than the ion drive thrust. The ion drive component of the system was dropped, and use of the concept of using the magnetic scoop as a magnetic sail or Magsail (MS) was born.[44]

Andrews & Zubrin Magsail

The figure shows the magsail design[4] consisting of a loop of superconducting wire of radius ${\displaystyle R_{c}}$ on the order of 100 km that carries a direct current ${\displaystyle I_{c}}$ that generates a magnetic field, which was modeled according to the Biot–Savart law inside the loop and as a magnetic dipole far outside the loop. With respect to the plasma wind direction a magsail may have a radial (or normal) orientation or an axial orientation that can be adjusted to provide torque for steering. In non-axial configurations lift is generated that can change the spacecraft's momentum. The loop connects via shroud lines (or tethers) to the spacecraft in the center. Because a loop carrying current is forced outwards towards a circular shape by its magnetic field, the sail could be deployed by unspooling the conductor wire and applying a current through it via the peripheral platforms.[6] The loop must be adequately attached to the spacecraft in order to transfer momentum from the plasma wind and would pull the spacecraft behind it as shown in the axial configuration in the right side of the figure.

Analysis of magsail performance was done using a simulation and a fluid (i.e., MHD) model with similar results observed for one case.[4] The magnetic moment of a current loop (A m²) is ${\displaystyle \mathbf {m} =I_{c}\pi R_{c}^{2}}$ for a current of ${\textstyle I_{c}}$ A and a loop of radius ${\textstyle R_{c}}$ m. Close to the loop, the magnetic field at a distance ${\displaystyle z}$ along the center-line axis perpendicular to the loop is derived from the Biot-Savart law as follows.[45]^{: sec 5-2, Eq (25)}

$${\displaystyle B_{cl}(z)={\frac {\mu _{0}I_{c}R_{c}^{2}}{2(z^{2}+R_{c}^{2})^{3/2}}}}$$

(MS.1)

At a distance far from the loop center the magnetic field is approximately that produced by a magnetic dipole. Te pressure at the magnetospheric boundary is doubled due to compression of the magnetic field and stated by the following equation at a point along the center-line axis or the target magnetopause standoff distance ${\displaystyle L_{Z}}$.[4]^{: Eq (5)}

${\displaystyle p_{mb}={\frac {B_{cl}(0)^{2}}{2\mu _{0}}}{\Biggl (}{\frac {R_{c}}{L_{Z}}}{\Biggr )}^{6}}$

(MS.2)

Equating this to the dynamic pressure for a plasma environment ${\textstyle p_{mb}=\rho \,u_{pe}^{2}/2}$, inserting ${\textstyle B_{cl}(0)}$ from equation MS.1 and solving for ${\displaystyle L_{Z}}$ yields[4]^{: Eq (6)}

${\displaystyle L_{Z}=1.26\,C_{Z},where\,\,C_{Z}=R_{c}{\Biggl (}{\frac {B_{cl}(0)}{u_{pe}{\sqrt {\rho \mu _{0}}}}}{\Biggr )}^{1/3}}$

(MS.3)

Andrews and Zubrin derived the drag (thrust) force of the sail ${\displaystyle F_{D}}$[4]^{: Eq (8)} that determined the characteristic length ${\displaystyle L_{Z}}$ for a tilt angle, but according to Freeland[7]^{: Sec 6.5} an error was made in numerical integration in choosing the ellipse downstream from the magnetopause instead of the ellipse upstream that made those results optimistic by a factor of approximately 3.1, which should be used to correct any drag(thrust) force results using[4]^{: Eq 8} Instead, this article uses the approximation[7]^{: Eq (108)} for a spherical bubble that corrects this error and is close to the analytical formula for the axial configuration as the force for the Magsail as follows

${\displaystyle F_{MS}=1.214\,\,{\frac {\rho u_{pe}^{2}}{2}}\pi \,L_{Z}^{2}}$

(MS.4)

In 2004 Toivanen and Janhunen did further analysis on the Magsail that they called a Plasma Free MagnetoPause (PFMP) that produced similar results to that of Andrews and Zubrin.[32]

The minimum required mass to carry the current in equation MS.1 or other magnetic sail designs from Andres/Zubrin (9)[4]^{: Eq (9)} and Crowl[46]^{: Eq (3)} as follows:

${\displaystyle _{min}M_{c}\,=2\,\pi \,R_{c}\,I_{c}\,/(J_{e}/\delta _{c})}$

(CMC.1)

where ${\displaystyle J_{e}}$ is the superconductor critical current density (A/m²) and ${\textstyle \delta _{c}}$ is the coil material density, for example ${\displaystyle J_{e}}$ = 1x10¹¹ A/m² and ${\textstyle \delta _{c}}$ = 6,500 kg/m³ for a superconductor in Freeland[7]^{: Apdx A} The physical mass of the coil is

${\displaystyle _{phy}M_{c}=(2\,\pi +N_{tether})\,R_{c}\,\pi \,r_{c}^{2}\,\delta _{c}}$

(CMC.2)

where ${\displaystyle r_{c}}$ is the radius of the superconductor wire, for example that necessary to handle the tension for a particular use case, such as deceleration in the ISM where ${\displaystyle r_{c}}$ = 10 mm.[7]^{: Apdx A} The ${\displaystyle N_{tether}}$ factor (e.g., 3) accounts for mass of the tether (or shroud) lines to connect the coil to a spacecraft. Note that ${\displaystyle _{phy}M_{c}}$ with ${\displaystyle N_{tether}}$=0 must be no less than ${\displaystyle _{min}M_{c}}$ in order for the coil to carry the superconductor critical current ${\displaystyle I_{cc}=J_{e}\pi r_{c}^{2}}$ amperes for a coil wire of radius ${\displaystyle r_{c}}$, for example ${\displaystyle I_{cc}}$ = 7,854 kiloampere (kA.)[7]^{: Apdx A}

Setting equation CMC.2 with ${\displaystyle N_{tether}}$=0 equal to equation CMC.1 and solving for ${\displaystyle r_{c}}$ yields the minimum required coil radius

${\displaystyle _{min}r_{c}={\sqrt {I_{c}/(J_{e}\pi )}}}$

(CMC.3)

If operated within the solar system, high temperature superconducting wire (HTS) is necessary to make the magsail practical since required current is large, millions of amperes. Protection from solar heating is necessary closer to the Sun, for example by highly reflective coatings.[47] If operated in interstellar space low temperature superconductors (LTS) could be adequate since the temperature of a vacuum is 2.7 Kelvins (K), but radiation and other heat sources from the spacecraft may render LTS impractical. The critical current ${\displaystyle I_{cc}}$ of the HTS YBCO coated superconductor wire increases at lower temperatures with a current density ${\displaystyle J_{e}}$ of 6x10¹⁰ A/m² at 77 K and 9x10¹¹ A/m² at 5 K.

The MHD applicability test of equation MHD.5 fails in some ISM deceleration cases and a kinematic model is necessary, such as the one documented in 2017 by Claudius Gros summarized here.[22] A spacecraft with an overall mass ${\displaystyle m_{tot}}$ and velocity ${\displaystyle v}$ follows [22]^{: Eq (1)} of motion as:

${\displaystyle F_{MKM}=m_{tot}{\dot {v}}=-\left(A_{G}(v)n_{p}v\right)(2m_{p}v)=2\,\rho _{im}\,v^{2}A_{G}(v),}$

(MKM.1)

where ${\displaystyle F_{MKM}}$ N is force predicted by this model, ${\displaystyle n_{p}}$ m⁻³ is the proton number density, ${\displaystyle m_{p}}$ kg is the proton mass, ${\displaystyle \rho =m_{p}n_{p}}$ kg/m³ the plasma density, and ${\displaystyle A_{G}(v)}$ m² the effective reflection area. This equation assumes that the spacecraft encounters ${\displaystyle A_{G}(v)n_{p}v}$ particles per second and that every particle of mass ${\displaystyle m_{p}}$ is completed reflected. Note that this equation is of the same form as MFM.5 with ${\displaystyle C_{d}}$=4, interpreting the ${\displaystyle C_{d}}$ term as just a number.

Gros numerically determined the effective reflection area ${\textstyle A_{G}(v)}$ by integrating the degree of reflection of approaching protons interacting with the superconducting loop magnetic field according to the Biot-Savart law. The reported result was independent of the loop radius ${\displaystyle R_{c}}$. An accurate curve fit as reported in Figure 4 to the numerical evaluation for the effective reflection area for a magnetic sail in the axial configuration from equation (8) was

${\displaystyle A_{G}(v)=0.081\pi R_{c}^{2}\left[\log \left({\frac {cI}{vI_{G}}}\right)\right]^{3}\,\,,v/c<I/I_{G}}$

(MKM.2)

where ${\displaystyle \pi R_{c}^{2}}$ is the area enclosed by the current carrying loop, ${\displaystyle c}$ the speed of light, and the value ${\displaystyle I_{G}=1.55\cdot 10^{6}}$A determined a good curve fit for ${\displaystyle I}$=10⁵ A, the current through the loop. In 2020, Perakis published an analysis[48] that corroborated the above formula with parameters selected for the solar wind and reported a force no more than 9% less than the Gros model for ${\displaystyle I}$=10⁵ A and ${\displaystyle R_{c}}$=100 m with the coil in an axial orientation.. That analysis also reported on the effect of magsail tilt angle on lift and side forces for a use case in maneuvering within the solar system.

For comparison purposes, the effective sail area determined for the magsail by Zubrin from equation MS.3 with the 3.1 correction factor from Freeland applied and using the same velocity value (resolving the discrepancy noted by Gros) as follows:

${\displaystyle A_{Z}(v)={\frac {1.124\times 1.26}{3.1}}\,L_{Z}}$

(MKM.3)

Magsail MHD and kinematic model effective sail area

The figure shows the normalized effective sail area normalized by the coil area ${\displaystyle \pi R_{c}^{2}}$ for the MKM case from Gros of equation MKM.1 and for Zubrin from equation MKM.3 for ${\displaystyle I\approx I_{G}}$, ${\displaystyle R_{c}}$=100 km, and ${\displaystyle n_{p}}$=0.1 cm⁻³ for the G-cloud on approach to Alpha Centauri corresponding to ISM density ${\displaystyle \rho _{im}=1.67\times 10^{-22}}$ kg/m³ consistent with that from Freeland[7] plotted versus the spacecraft velocity relative to the speed of light ${\textstyle \beta =v/c}$. A good fit occurs for these parameters, but for different values of ${\displaystyle R_{c}}$ and ${\displaystyle I}$ the fit can vary significantly. Also plotted is the MHD applicability test of ion gyroradius divided by magnetopause radius ${\displaystyle r_{g}/R_{mp}}$ <1 from equation MHD.4 on the secondary axis. Note that MHD applicability occurs at ${\displaystyle v/c}$ < 1%. For comparison, the 2004 Fujita ${\displaystyle C_{d}}$ as a function of ${\displaystyle r_{g}/R_{mp}}$ from the MHD applicability test section is also plotted. Note that the Gros model predicts a more rapid decrease in effective area than this model at higher velocities. The normalized values of ${\displaystyle A_{G}(v)}$ and ${\displaystyle A_{Z}(v)}$ track closely until ${\displaystyle \beta =v/c\approx }$ 10% after which point the Zubrin magsail model of Equation MS.4 becomes increasingly optimistic and equation MKM.2 is applicable instead. Since the models track closely up to ${\displaystyle \beta \approx }$ 10%, with the kinematic model underestimating effective sail area for smaller values of ${\displaystyle \beta }$ (hence underestimating force), equation MKM.1 is an approximation for both the MHD and kinematic region. The Gros model is pessimistic for ${\displaystyle \beta }$ < 0.1%.

Gros used the analytic expression for the effective reflection area ${\displaystyle A_{G}(v)}$ from equation MKM.3 for explicit solution for the required distance ${\displaystyle x_{f}}$ m to decelerate to final velocity ${\displaystyle v_{f}\approx 0.013c}$ m/s from [22]^{: Eq (10)} given an initial velocity ${\displaystyle v_{0}}$ m/s for a spacecraft mass ${\displaystyle m_{tot}}$ kg as follows:

${\displaystyle x_{f}={\frac {m_{tot}\,[g(v_{0})-g(v_{f})]}{0,081\,m_{p}\,n_{p}\pi \,R_{c}^{2}}}}$

(MKM.4)

where ${\textstyle g(v)=ln^{-2}({\frac {v\,I_{G}}{c\,I}})}$. When ${\displaystyle v_{f}}$=0 the above equation is defined in [22]^{: Eq (11)} as ${\displaystyle x_{max}}$, which enabled a closed form solution of the velocity at a distance ${\displaystyle x,v(x)}$ in [22]^{: Eq (12)} with numerical integration required to compute the time required to decelerate.[22]^{: Eq (14)} Equation (16) The optimal current that minimized ${\displaystyle x_{max}}$ as ${\displaystyle I_{opt}=e\beta _{0}I_{G}}$ where ${\displaystyle \beta _{0}=v_{0}/c}$.[22]^{: Eq (16)} In 2017 Crowl[46] optimized coil current for the ratio of effective area ${\displaystyle A(v)}$ over total mass ${\displaystyle m_{tot}}$ and derived the result ${\displaystyle I_{opt}=e^{3}\,\beta _{0}I_{G}}$.[22]^{: Eq (15)} That paper used results from Gros for the stopping distance ${\displaystyle x_{max}}$ and time to decelerate.

Magsail ISM deceleration distance and time comparison

The figure plots the distance traveled while decelerating ${\displaystyle x_{d}}$ and time required to decelerate ${\displaystyle t_{d}}$ given a starting relative velocity ${\displaystyle \beta _{0}=v_{0}/c}$ and a final velocity ${\displaystyle v_{f}=0.013c}$ m/s consistent with that from Freeland[7] for the same parameters above. Equation CMC.1 gives the magsail mass ${\displaystyle M_{s}}$ as 97 tonnes assuming payload mass ${\displaystyle M_{p}}$ of 100 tonnes using the same values used by Freeland[7] of ${\displaystyle J_{e}}$ = 10¹¹ A/m² and ${\displaystyle \delta _{c}}$=6,500 kg/m³ for the superconducting coil. Equation MS.4 gives Force for the magsail multiplied by ${\displaystyle C_{d}}$=4 for the Andrews/Zubrin model to align with equation MHD.3 definition of force from the Gros model. Acceleration is force divided by mass, velocity is the integral of acceleration over the deceleration time interval ${\displaystyle t_{d}}$ and deceleration distance traveled ${\displaystyle x_{d}}$ is the integral of the velocity over ${\displaystyle t_{d}}$. Numerical integration resulted in the lines plotted in the figure with deceleration distance traveled plotted on the primary vertical axis on the left and time required to decelerate on the secondary vertical axis on the right. Note that the MHD Zubrin model and the Gros kinematic model predict nearly identical values of deceleration distance up to ${\displaystyle \beta _{0}}$~ 5% of c, with the Zubrin model predicting less deceleration distance and shorter deceleration time at greater values of ${\displaystyle \beta _{0}}$. This is consistent with the Gros model predicting a smaller effective area ${\displaystyle A(v)}$ at larger values of ${\displaystyle \beta _{0}}$. The value of the closed form solution for deceleration distance ${\displaystyle x_{f}}$from MKM.4 for the same parameters closely tracks the numerical integration result.

Dana Andrews and Robert Zubrin first proposed the magnetic sail concept in 1988 for interstellar travel for acceleration by a fusion rocket, coasting and then deceleration via a magsail at the destination that could reduce flight times by 40–50 years[3] In1989 details for interplanetary travel were reported[4] In 1990 Andrews and Zubrin reported on an example for solar wind parameters one AU away from the Sun, with ${\textstyle n_{i}=5\times 10^{6}}$ m⁻³ with only protons as ions, apparent wind velocity ${\textstyle u_{sw}}$=500 km/s the field strength required to resist the dynamic pressure of the solar wind is 50 nT from equation MHD.2. With radius ${\displaystyle R_{c}}$=100 km and magnetospheric bubble of ${\textstyle L}$=500 km (310 mi) reported a thrust of 1980 newtons and a coil mass of 500 tonnes.[35] For the above parameters with the correction factor of 3.1 applied to equation MS.4 yields the same thrust and equation CMC.1 yields the same coil mass. Results for another 4 solar wind cases were reported,[4] but the MHD applicability test of equation MHD.5 fails in these cases.

In 2015 Freeland documented a use case with acceleration away from Earth by a fusion drive with a magsail used for interstellar deceleration on approach to Alpha Centaturi as part of a study to update Project Icarus[7] with ${\displaystyle R_{c}}$=260 km, an initial ${\textstyle R_{mp}}$ of 1,320 km and ISM density ${\displaystyle \rho _{im}=1.67\times 10^{-22}}$ kg/m³, almost identical to the n(H I) measurement of 0.098 cm⁻³ by Gry in 2014.[30] The Freeland study predicted deceleration from 5% of light speed in approximately 19 years. The coil parameters ${\displaystyle J_{e}}$=10¹¹ A/m², ${\displaystyle r_{sc}}$= 5 mm, ${\displaystyle \rho _{sc}}$=6,500 kg/m³, resulted in an estimated coil mass of ${\displaystyle M_{c}(phy)}$=1,232 tonnes. Although the critical current density ${\displaystyle J_{e}}$ was based upon a 2000 Zubrin NIAC report projecting values through 2020, the assumed value is close to that for commercially produced YBCO coated superconductor wire in 2020. The mass estimate may be optimistic since it assumed that the entire coil carrying mass is superconducting while 2020 manufacturing techniques place a thin film on a non-superconducting substrate. For the interstellar medium plasma density ${\displaystyle \rho _{im}}$=1.67x10⁻²² with an apparent wind velocity 5% of light speed, the ion gyroradius is 570 km and thus the design value for ${\textstyle R_{mp}}$ meets the MHD applicability test of equation MHD.5. Equation MFM.3 gives the required coil current as ${\displaystyle I_{c}}$~7,800 kA and from equation CMC.1 ${\displaystyle M_{c}(min)}$= 338 tonnes; however, but the corresponding superconducting wire minimum radius from equation CMC.3 is ${\displaystyle r_{c}(min)}$ =1 mm, which would be insufficient to handle the decelerating thrust force of ${\displaystyle F_{MS}}$ ~ 100,000 N predicted by equation MS.4 and hence the design specified ${\displaystyle r_{sc}}$= 5 mm to meet structural requirements. In a complete design, the mass of infrastructure, including coil shielding to maintain critical temperature and survive abrasion in outer space, must also be included. Appendix A estimates these as 90 tonnes for wire shielding and 50 tonnes for the spools and other magsail infrastructure. Freeland compared this magsail deceleration design with one where both acceleration and deceleration were performed by a fusion engine and reported that the mass of such a "dirty Icarus" design was over twice that of a magsail used for deceleration. An Icarus design published in 2020 used a Z-pinch fusion drive in an approach called Firefly that dramatically reduced mass of the fusion drive and made fusion only drive performance for acceleration and deceleration comparable to the fusion for acceleration and magsail for deceleration design.[49]

In 2017 Gros[22] reported numerical examples for the Magsail kinematic model that used different parameters and coil mass models than those used by Freeland. That paper assumed hydrogen ion (H I) number densities of 0.05-0.2 cm⁻³ (9x10⁻²³ - 3x10⁻²² kg/m³) for the warm local clouds[50] and about 0.005 cm⁻³ (9x10⁻²³ kg/m³) for voids of the local bubble.[51] Patches of cold interstellar clouds with less than 200 AU may have large densities of neutral hydrogen up to 3000 cm⁻³ ,which would not respond to a magnetic field.[52] For a high speed mission to Alpha Centauri with initial velocity before deceleration ${\displaystyle v_{0}=c/10}$ using a coil mass of 1500 tons and a coil radius of ${\displaystyle R}$=1600 km, the estimated stopping distance ${\displaystyle x_{max}}$ was 0.37 light years and the total travel time of 58 years with 1/3 of that being deceleration.

In 2017 Crowl documented a design for a mission starting near the Sun and destined for Planet nine approximately 1,000 AU distant[46] that employed the Magsail kinematic model. The design accounted for the Sun's gravity as well as the impact of elevated temperature on the superconducting coil, composed of meta-stable metallic hydrogen, which has a mass density of 3,500 kg/m³ about half that of other superconductors. The mission profile used the Magsail to accelerate away from 0.25 to 1.0 AU from the Sun and then used the Magsail to brake against the Local ISM on approach to Planet nine for a total travel time of 29 years. Parameters and coil mass models differ from those used by Freeland.

Another mission profile uses a magsail oriented at an attack angle to achieve heliocentric transfer between planets moving away from or toward the Sun. In 2013 Quarta and others[53] used Kajimura 2012 simulation results[41] that described the lift (steering angle) and torque to achieve a Venus to Earth transfer orbit of 380 days with a coil radius of ${\displaystyle R_{c}}$~1 km with characteristic acceleration ${\displaystyle a_{c}}$=1 mm/s². In 2019 Bassetto and others[54] used the Quarta "thick" magnetopause model and predicted a Venus to Earth transfer orbit of approximately 8 years for a coil radius of ${\displaystyle R_{c}}$~1 km. with characteristic acceleration ${\displaystyle a_{c}}$=0.1 mm/s². In 2020 Perakis[48] used the Magsail kinematic model with a coil radius of ${\displaystyle R_{c}}$=350 m, current ${\displaystyle I_{c}}$=10⁴ A and spacecraft mass of 600 kg that changed attack angle to accelerate away from the Earth orbit and decelerate to Jupiter orbit within 20 years.

Winglee M2P2 schematic

In 2000 Winglee, Slough and others proposed a design order to reduce the size and weight of a magnetic sail and named it mini-magnetospheric plasma propulsion (M2P2).[8] The figure based upon[8][55][56][10] illustrates the M2P2 design, which was the basis of the Magneto plasma sail (MPS) design. Starting at the center with a solenoid coil of radius ${\displaystyle R_{H}}$ of ${\textstyle N_{t}}$=1,000 turns carrying a radio frequency current that generates a helicon[57] wave that injects plasma fed from a source into a coil of radius ${\textstyle R_{c}}$ that carries a current of ${\displaystyle I_{c}}$, which generates a magnetic field. The excited injected plasma enhances the magnetic field and generates a miniature magnetosphere around the spacecraft, analogous to the heliopause where the Sun injected plasma encounters the interstellar medium, coronal mass ejections or the Earth's magnetotail. The injected plasma created an environment that analysis and simulations showed had a magnetic field with a falloff rate of ${\displaystyle 1/r}$ as compared with the classical model of a ${\textstyle 1/r^{3}}$ falloff rate, making the much smaller coil significantly more effective.[8][58] The pressure of the inflated plasma along with the stronger magnetic field pressure at a larger distance due to the lower falloff rate would stretch the magnetic field and more efficiently inflate a magnetospheric bubble around the spacecraft.