And the Spirit & the bride say, come.... Reveaaltion 22:17

And the Spirit & the bride say, come.... Reveaaltion 22:17
And the Spirit & the bride say, come...Revelation 22:17 - May We One Day Bow Down In The DUST At HIS FEET ...... {click on blog TITLE at top to refresh page}---QUESTION: ...when the Son of man cometh, shall he find faith on the earth? LUKE 18:8

Saturday, August 28, 2021

Creation Moment 8/29/2021 - More "TOI's" of Creator's Skies

"Astronomers have discovered five transiting companions near the
hydrogen-burning mass limit in close orbits around main-sequence stars TOI-148, TOI-587, TOI-681, TOI-746, and TOI-1213.
A defining characteristic of brown dwarfs is their relative low occurrence rate (less than 1%) in close orbits (less than 5 AU) around main-sequence stars compared to giant planets and other stars, or the ‘brown dwarf desert.’
Brown dwarfs are supposed to shrink over time as they burn up their deuterium reserves and cool down,” said Professor François Bouchy.
We found that the two oldest objects, TOI-148b and TOI-746b, have a smaller radius, while the two younger companions have larger radii.
With an effective temperature of 9800 ± 200 K, TOI-587 is the hottest known main-sequence star to host a transiting brown dwarf or very low-mass star. We found evidence of spin-orbit synchronization for TOI-148 and TOI-746 as well as tidal circularization for TOI-148.
Even with these additional objects, we still lack the numbers to draw definitive conclusions about the differences between brown dwarfs and low-mass stars,” Dr. Grieves said.
 
TOI-681 has been previously reported to be a member of the open star cluster NGC 2516...TOI-681 is relatively hot (Teff = 7440 K) and fast rotating (Prot∕sin i = 2.61 ± 0.13 days) star, which can create enhanced magnetic fields from spin-orbit tidal synchronization for short period systems and has been thought to cause inflated radii of similar low-mass companions. However, given its relatively long period of 15.78 days TOI-681b is unlikely to have reached spin-orbit synchronization. 
 
TOI-746 .... with a companion on a moderately eccentric e = 0.199 ± 0.003 orbit. As discussed, tidal torques can drive a star’s rotation rate toward a tidally locked state where the tidal torques fix the rotation period Prot to the equilibrium rotation period Peq. Tidal models can predict Peq including the “constant phase lag” equilibrium tidal model. Following Barnes (2017) and Fleming et al. (2019) the CPL model permits a 1:1 and 3:2 spin-orbit state by:

Using the second case we find Peq = 7.32 days for TOI-746 and with an upper limit on the rotation period of Prot∕sin i = 7.9 ± 1.6 days TOI-746 may be in a supersychronous 3:2 spin-orbit state. We also consider the system may be in a pseudo-synchronous rotation state that approximates spin-orbit synchronization around the time of periastron. Zimmerman explored possible pseudosynchronization for heartbeat binary stars with Kepler lightcurves but found generally that their sampleclustered around times the pseudosynchronization period indicating that they have plateaued prematurely in their synchronization. We roughly estimate this using Kepler’s third law to determine what the period would be if the companion was in a circular orbit at the periastron distance: 

Assuming this circular orbit at periastron we find Pperi = 7.88 ± 0.05 days which is very similar to the upper limit of the rotation period suggesting TOI-746 may be in a pseudo-synchronous rotation at periastron.

TOI-1213 ... star with a companion on an eccentric e = 0.498 orbit. We find Peq = 18.14 days for TOI-1213, and with Prot∕sin i = 12.0 ± 3.6 days TOI-1213 does not appear to have spin-orbit synchronization. 

TOI-148,which is on the upper end of v sin i* distributions for stars of similar mass, indicating TOI-148’s stellar rotation period may be affected by tidal torques with its companion. 

TOI-587 is a very hot star which is outside the range of temperatures in the spectral library of SpecMatch-Emp. TOI-587 also falls outside the valid temperature range for the MARCS model atmospheres and we instead use the ATLAS9 model atmosphere..... TOI-587 is the hottest main-sequence host star of a transiting brown dwarf or low-mass star below 150 MJup  with a Teff = K. 

The sample of transiting brown dwarfs and low-mass stars we analyzed is still too small to make significant statistical claims; however, their eccentricity and metallicity distributions are still consistent with previous suggestions of two separate populations for lower and higher mass brown dwarfs." SciNews/ecosciences
Maybe they were CREATED as two different star Populations... Which commandeth the sun, and it riseth not; and sealeth up the stars. Job 9:7