Abid is the hare who runs fast and takes long rest while Gautam runs slow but takes short rest. Abid can run at 5 ms−1 while Gautam runs at 3 ms−1 . Abid has to take a 10s break after running 20s. But Gautam can take a 10s break after 90s. They are running a 1km (1000 m) race. What is the time difference between winner and loser? (Write the value in seconds upto nearest whole number)

Guatam is the fastest the other was the slowest

Abid
Velocity = 3 m/s
Can take a break for = 10s
Takes a break after = 20s

Time taken to run 1000m without breaks = 1000/5 = 200s

Abid takes 200s to run 1km without any breaks

If he takes a break after every 20s,
Then, number of breaks he takes = 200s/20s = 10 breaks

Time he spend in every break = 10s
Amount of time spent specifically in breaks = 10breaks * 10 s = 100s
Time inclusive of breaks = 200s + 100s = 300s

Hence Abid takes 300s with breaks

Gautam
Velocity = 3 m/s
He can take a break for 10s
He has to take a break after running 90s

Time taken without breaks = 1000m / 3 ms-1 = 333.3s
Time taken for Gautam to cover 1km without any breaks = 333.3s

He can take a break after running for 90s
Number of brakes he can take = 333.3s / 90s = 3.703 breaks
He can take 3.703 breaks in his entire journey

Amount of time he can spend in his break = 10s
Amount of time wasted = 3.703breaks * 10s = 37.03s

Total time = 333.3s + 37.03s = 370.39s

Rounding off = 370s
Hence, Gautam reaches the end of 1km faster than 1km

Difference = 370s - 300s = 70s

Hope it’s right

  sequence  is a continuous and distinctive band of  stars  that appears on plots of stellar  color  versus  brightness. these color-magnitude plots are known as  hertzsprung–russell diagramsafter their co-developers,  ejnar hertzsprungand  henry norris russell. stars on this band are known as  main-sequence stars  or  dwarf stars. these are the most numerous true stars in the universe, and include the earth's  sun.after condensation and ignition of a star, it generates  thermal energy  in its dense core region through  nuclear fusion  of  hydrogen  into  helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in  hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of  gravitational collapse  from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the  photosphere. the energy is carried by either  radiation  or  convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the  mass of the sun  (1.5  m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the  proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of  carbon,  nitrogen  and  oxygen  as intermediaries in the  cno cycle  that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4  m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star  evolves  away from the main sequence on the hr diagram, into a  supergiant,  red giant, or directly to a  white dwarf.