Editing Magnetic sail (section)

=== Acceleration/deceleration in a stellar plasma wind ===
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.<ref name=":0">{{Cite journal |last=Djojodihardjo |first=Harijono |date=21 November 2018 |title=Review of Solar Magnetic Sailing Configurations for Space Travel |url=https://www.researchgate.net/publication/329103132 |journal=Advances in Astronautics Science and Technology |volume=2018 |issue=1 |pages=207–219 |bibcode=2018AAnST...1..207D |doi=10.1007/s42423-018-0022-4 |s2cid=125294757|doi-access=free }}</ref> Near the Earth's orbit at 1 AU the plasma flows at velocity <math>v_{sw}</math> dynamically ranges from 250 to 750&nbsp;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<ref>{{Cite web |last=NOAA |date= |title=REAL TIME SOLAR WIND |url=https://www.swpc.noaa.gov/products/real-time-solar-wind |access-date=June 12, 2022}}</ref> Assuming that 8% of the solar wind is helium and the remainder hydrogen, the average solar wind plasma mass density at 1 AU is <math>4\times10^{-21}<\rho_{sw}(1)<10^{-20}</math> kg/m<sup>3</sup> (typically 10<sup>−20</sup> kg/m<sup>3</sup>).<ref>{{Cite web |date=June 29, 2022 |title=Solar Wind |url=https://umbra.nascom.nasa.gov/spartan/the_solar_wind.html |access-date=June 29, 2022 |website=umbra.nascom.nasa.gov}}</ref>

The average plasma mass density of ions <math>\rho_{sw}</math> decreases according to an [[Inverse-square law]] with the distance from the Sun as stated by Andrews/Zubrin<ref name=":4" />  and Borgazzi.<ref name=":32" /> The velocity for values near the Sun is nearly constant, falling off slowly after 1 AU<ref name=":32">{{Cite journal |last1=Borgazzi |first1=A. |last2=Lara |first2=A. |last3=Echer |first3=E. |last4=Alves |first4=M. V. |date=May 2009 |title=Dynamics of coronal mass ejections in the interplanetary medium |url=http://www.aanda.org/10.1051/0004-6361/200811171 |journal=Astronomy & Astrophysics |volume=498 |issue=3 |pages=885–889 |bibcode=2009A&A...498..885B |doi=10.1051/0004-6361/200811171 |issn=0004-6361}}</ref>{{Rp|location=Fig 5}} and then rapidly decreases at [[Heliosphere#Edge structure|heliopause]].