Hot Jupiters ( HJs ) are Jupiter-like planets that reside very closely to their host star , within \sim 0.1 \mathrm { AU } .
Their formation is not well understood .
It is generally believed that they can not have formed in situ , implying that some form of migration must have occurred after their initial formation .
We study the production of HJs through secular evolution in multiplanet systems with three to five planets .
In this variant of high- e migration , the eccentricity of the orbit of the innermost planet is excited on secular time-scales , triggering orbital migration due to tidal dissipation .
We use a secular dynamics code and carry out a population synthesis study .
We find that HJs are only produced if the viscous time-scale is short ( \approx 0.014 yr ) .
In contrast , in up to \approx 0.3 of systems , the innermost planet is tidally disrupted .
The orbital period distribution is peaked around 5 d , consistent with observations .
The median HJ mass is 1 M _ { \mathrm { J } } with a maximum of \approx 2 M _ { \mathrm { J } } , similar to observed HJs .
Approximately 0.1 of the HJs have retrograde orbits with respect to the stellar spin .
We do not find a significant population of warm Jupiters in our simulations , i.e .
planets with semimajor axes between 0.1 and 1 AU .