FANDOM


  1. Modify common6.h and include under COMMON/NBODY/ the line
         &               LMNST(NMAX), RDS(NMAX)

    This will introduce global arrays in which luminosity and stellar radius of each star are going to be stored during the simulation.

  2. Modify hrplot.f and include the following lines just above the last WRITE statements for unit 82:
    * Store LUM & RM globally for xnbody	      
    	      LMNST(J1)=LUM
    	      LMNST(J2)=LUM2
    	      RDS(J1)=RM
    	      RDS(J2)=RM2

    and unit 83:

    * Store LUM & RM globally for xnbody	      
    	      LMNST(I)=LUM
    	      RDS(I)=RM

    At the end of hrplot, set the output frequency DTPLOT in Myr (default: 10.0). The end of hrplot.f should look something like this:

    *       Update plot interval (10 Myr initially) and next output time.
          IF (TIME.EQ.0.0D0) THEN
              DTPLOT = 10.0
              TPLOT = TPLOT + DTPLOT/TSTAR
          END IF
          TPLOT = TPLOT + DTPLOT/TSTAR
          CALL FLUSH(82)
          CALL FLUSH(83)
    *
          RETURN
    *
          END
  3. Modify viscon.f, in particular the subroutine VISCONPART:
                    VBUFFER(21,LSTORED)=LOG10((LMNST(I)/(RDS(I)**2))**0.25)
                    VBUFFER(22,LSTORED)=LOG10(REAL(LMNST(I)))

    Now temperature (which is a function of luminosity and stellar radius according to the Stefan-Boltzmann law) and luminosity are stored in the attributes ATT4 and ATT5.

  4. Compile nbody6++ with xnbody/VISIT support.
  5. In your nbody6++ input file, turn on stellar evolution by setting KZ(12)=1 and KZ(19)=3.
  6. Start nbody6++ and xnbody and make the 2D plot windows display ATT5 against ATT4.

Ad blocker interference detected!


Wikia is a free-to-use site that makes money from advertising. We have a modified experience for viewers using ad blockers

Wikia is not accessible if you’ve made further modifications. Remove the custom ad blocker rule(s) and the page will load as expected.