We examine the implications of Modified Newtonian Dynamics ( MOND ) on the large scale structure in a Friedmann-Robertson-Walker universe .
We employ a “ Jeans swindle ” to write a MOND-type relationship between the fluctuations in the density and the gravitational force , { \bf g } .
In linear Newtonian theory , | { \bf g } | decreases with time and eventually becomes < g _ { { } _ { 0 } } , the threshold below which MOND is dominant .
If the Newtonian initial density field has a power-law power-spectrum of index n < -1 , then MOND domination proceeds from small to large scale .
At early times MOND tends to drive the density power-spectrum towards k ^ { -1 } , independent of its shape in the Newtonian regime .
We use N-body simulations to solve the MOND equations of motion starting from initial conditions with a CDM power-spectrum .
MOND with the standard value g _ { { } _ { 0 } } = 10 ^ { -8 } { \mathrm { c } m s ^ { -2 } } , yields a high clustering amplitude that can match the observed galaxy distribution only with strong ( anti- ) biasing .
A value of g _ { { } _ { 0 } } \approx 10 ^ { -9 } { \mathrm { c } m s ^ { -2 } } , however , gives results similar to Newtonian dynamics and can be consistent with the observed large scale structure .