Open AccessModified Newtonian dynamics of large‐scale structure
Author(s) -
Nusser Adi
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05235.x
Subject(s) - physics , modified newtonian dynamics , astrophysics , dark matter , spectral density , galaxy , newtonian dynamics , gravitation , power law , amplitude , newtonian fluid , cold dark matter , structure formation , classical mechanics , galaxy rotation curve , quantum mechanics , galaxy formation and evolution , statistics , mathematics
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, g . In linear Newtonian theory, | 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 the small to the 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 cold dark matter (CDM) power spectrum. MOND with the standard value g 0 =10 ‐8 cm s ‐2 yields a high clustering amplitude that can match the observed galaxy distribution only with strong (anti‐) biasing. A value of g 0 ≈10 ‐9 cm s ‐2 , however, gives results similar to Newtonian dynamics and can be consistent with the observed large‐scale structure.