Gravitational 3-body interaction among binary stars and the supermassive black hole ( SMBH ) at the center of the Milky Way occasionally ejects a hypervelocity star ( HVS ) with a velocity of \sim 1000 \mathrm { km s } ^ { -1 } .
Due to the ejection location , such a HVS initially has negligible azimuthal angular momentum L _ { z } \simeq 0 \mathrm { kpc } \mathrm { km s } ^ { -1 } .
Even if the halo is mildly triaxial , L _ { z } of a recently ejected nearby HVS remains negligible , since its flight time from the Galactic center is too short to accumulate noticeable torque .
However , if we make a wrong assumption about the Solar position and velocity , such a HVS would apparently have noticeable non-zero angular momentum , due to the wrong reflex motion of the Sun .
Conversely , with precise astrometric data for a nearby HVS , we can measure the Solar position and velocity by requiring that the HVS has zero angular momentum .
Based on this idea , here we propose a method to estimate the Galactocentric distance of the Sun R _ { 0 } and the Galactocentric Solar azimuthal velocity V _ { \odot } by using a HVS .
We demonstrate with mock data for nearby HVS candidate ( LAMOST-HVS1 ) that the Gaia astrometric data , along with the currently available constraint on V _ { \odot } / R _ { 0 } from the proper motion measurement of Sgr A* , can constrain R _ { 0 } and V _ { \odot } with uncertainties of \sim 0.27 \mathrm { kpc } and \sim 7.8 \mathrm { km s } ^ { -1 } ( or fractional uncertainties of 3 \% ) , respectively .
Our method will be a promising tool to constrain ( R _ { 0 } ,V _ { \odot } ) , given that Gaia is expected to discover many nearby HVSs in the near future .