The present paper reviews selected aspects of the Guliyev ’ s hypothesis about the massive celestial body at a distance of 250–400 AU from the Sun as well as the factor of comets transfer . The analysis covers 1249 comets observed up to 2017 , having perihelion and aphelion distances greater than 0.1 and 30 AU respectively . It is shown , that the conjecture of the point around which cometary perihelia might be concentrated , is not consistent . On the issue of perihelia distribution , priority should be given to the assumption that there is a plane or planes around which the concentration takes place . The search engine for such planes was applied to numerous cometary groups , separated by clusters T ( discover date ) , e , q , H ( absolute magnitude ) , Q , 1 / a _ { ori } , etc . A total of 24 comet groups were investigated . In almost all cases there are detected two types of planes or zones : the first one is very close to the ecliptic , another one is about perpendicular to it and has the parameters : i _ { p } = 86 ^ { \circ } , \Omega _ { p } = 271.7 ^ { \circ } . The existence of the first area appears to be related to the influence of giant planets . The Guliyev ’ s hypothesis says that there is a massive perturber in the second zone , at a distance of 250–400 AU . It shows that number of aphelia and distant nodes of cometary orbits in this interval ( within statistical confidence ) significantly exceeds the expected background . Analysis of the angular parameters of the comets , calculated relative to the second plane ( reference point is the ascending node of a large circle ) displays clear patterns : shortage of comets near i ^ { \prime } = 180 ^ { \circ } , excess of them near B’ = 0 ^ { \circ } ( ecliptic latitude of perihelion ) and shortage near B’ = -90 ^ { \circ } . The analysis also shows irregularity of distant nodes , overpopulation of perihelion longitudes in the range 350 ^ { \circ } – 20 ^ { \circ } . Plotted distributions of aphelia N ( Q ) and distant cometary nodes clearly indicate a perturbation of the natural course near 300 AU . On the basis of collected cometary data , we have estimated orbital elements of the hypothetical planetary body : a = 337 \mathrm { AU } ;\ > e = 0.14 ;\ > \omega = 57 ^ { \circ } ;\ > \Omega = 272.7 ^ { \circ } ;\ > i = 86 ^ % { \circ } Naturally , each value may contain some errors . In order to test the stability of such an orbit , the planet was integrated for 10 ^ { 7 } yr , assuming that its mass is about \sim 10 M _ { \oplus } . The orbits of 33 comets ( having aphelia and distant nodes 286–388 AU ) are also integrated in the past for a million years in order to trace possible dynamic relationship with the planet . In doing so , we varied the mean anomaly of the planet from 0 ^ { \circ } to 360 ^ { \circ } by 10 ^ { \circ } in each cycle of numerical explorations . A number of close encounters between comets and the hypothetical body have been discovered .