Electro wrote:JeffreyW wrote:
In this theory it is easy to form smaller objects. A gas object that gets ripped apart too quickly would not have enough time to form a large object in its interior. It would deposit very little before the thick atmosphere is ripped away.
Ripped away how?
First thank you for asking the question. It does help me considerably to review and hone the theory when people as me questions concerning it.
Orbiting too close to a hotter star. Think of a pot of water on the stove. The water will boil away if it is on the stove and it is hot and burning.
If the pot of water is in orbit around the stove and nowhere near it, the heat will not evaporate away the water. I guess that could be a simple demonstration. The same with older stars. If you stick one too close to a hotter host, it will evaporate away. I have outlined this into two types of principles:
Mass independence[edit]
A birthing star does not leave significant remains after it is born according to the coherency principle. This means the mass of the companion is not determined by the mass of the host in any fashion and cannot be explained with any mechanism which tries to connect the two. Therefore the mass independence principle of stellar formation can be stated quite clearly,
"The masses of stars are independent of each other when they are first formed/born."[130]
Mass dependence[edit]
The only time that the masses of stars will become even partially dependent on their hosts, is if they are orbiting at a somewhat close distance, and their atmospheres and material are being ripped away by the hotter hosts. This means the mass-dependence principle can be written as,
"The mass of a star is partially dependent on its host during its evolution if the orbital parameters can cause mass loss of the companion."[131]
The paper outlining the principles is here:
http://vixra.org/pdf/1607.0191v1.pdf
Abstract: In the recent paper, “KELT-17b: A Hot-Jupiter Transiting an A-Star in a Misaligned Orbit
Detected with Doppler Tomography”, it is referenced that, “a sample of well characterized planets
around massive stars is necessary to understand the mass-dependence of planet properties.” Two
principles are provided to explain that mass-dependence attributed to formation processes is moot.
Explanation is provided.
On page 2, the paper states, “a sample of well characterized planets around massive stars is
necessary to understand the mass-dependence of planet properties.” What they mean is that they think
massive stars form at the same time as their companions in protoplanetary disks, and depending on how
massive the objects are which orbit their hosts they will be able to somehow explain how they formed.
The problem is that their assumption directly contradicts the coherency principle of stellar evolution,
"When a star is born its remains are incoherent particles that cannot form anything of significant size, as
stellar birthing is too violent to allow for the classical mode of planet formation in a protoplanetary disk.”
A birthing star does not leave significant remains after it is born according to the coherency
principle. This means the mass of the companion is not determined by the mass of the host in any
fashion and cannot be explained with any mechanism which tries to connect the two. Therefore the mass
independence principle of stellar formation can be stated quite clearly,
“The masses of stars are independent of each other when they are first formed/born.”
The only time that the masses of stars will become even partially dependent on their hosts, is if
they are orbiting at a somewhat close distance, and their atmospheres and material are being ripped
away by the hotter hosts. This means the mass-dependence principle can be written as,
“The mass of a star is partially dependent on its host during its evolution if the orbital parameters can
cause mass loss of the companion.”
This all means that characterizing older evolved stars (KELT-14b) around massive, young A-type
stars (KELT-14) by their mass will not lead to any understanding of their formation. This is
because in the KELT-14 system the A-type star is very young, and the Hot Jupiter which orbits as its
companion is very, very old and is having its atmosphere ripped away. Eventually it will expose its
rocky/ocean covered differentiated core left over to continue orbiting it. They will co-evolve indefinitely
according to the principle of stellar co-evolution and the young A-star will move down the line of its
evolution as well, becoming cooler and smaller, losing mass and possibly allowing for its companion to
host life on its surface.