Is Earth a Circumbinary planet ?
Andre Willers
25 Mar 2014
Synopsis :
If Sol is a binary star , with the companion (SolB) inside
SolA , it would explain a lot of things .
Discussion :
1.A watery planet in a circumbinary
orbit will tend to move into the goldilocks zone and stay there .
2. Why ?
Close binaries will spiral into each
other from friction .
Postulate a watery planet in
circumbinary orbit that is not unstable (ie 2 to 4 away from the center of
stellar mass than the distance between StarA and StarB .
Magnetic and electric forces are
maximal when water is liquid . This balances the rotational speed of the two
stars .
This sounds insufficient, but consider
leverage . And leverage is applicable . Even a small force from an orbiting
planet that swings wide leverages it onto the central binaries .
In other words , the binary stars
slows down in their orbit around each other and planet spirals outward the until the planet reaches maximal liquidity of
water .
If the planet goes out of goldilocks ,
it starts freezing , the stars start spiralling
inwards again and the planet moves back into the goldilocks zone .
It is stable .
3. Virtual Stars .
A star with a companion inside it can
be kept stable as a binary if there are watery or at least magnetic planets in
circumbinary orbits . The companion can be seen as a virtual star .
4.The habitability zone would then be
more like a magnetron . A regular fluctuation .
5. This is exactly what we observe .
Only we call it Kondratieff , etc , etc .
6. This would mean that habitable
planets are a dime-a-dozen .
7. If Sol is a Virtual Binary , then
climate prediction should be a snap .
8. Actually , one could say
immediately that the present climate warming is mostly due to the lobe of
habitability rotating past the Earth’s present position . The period seems to
be 400 years . Too aggressive cooling measures will saddle your descendants with
an ice-age in about 300 years. If any are still alive .
Aren’t Virtual Stars fun ?
Regards
Andre
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Appendix A
A circumbinary planet is a planet that orbits two stars instead
of one. Because of the short orbits of some binary stars, the only way for planets to form
is by forming outside the orbit of the two stars.[1] As of 5 December 2013, there
are seventeen confirmed systems of circumbinary planets.[2][3]
Contents
[show]
The first confirmed circumbinary extrasolar planet was found
orbiting the system PSR B1620-26, which
contains a millisecond pulsar and
a white dwarf and is located in the globular clusterM4. The existence of the third body was first
reported in 1993,[4] and was suggested to be a
planet based on 5 years of observational data.[5] In 2003 the planet was
characterised as being 2.5 times the mass of Jupiter in a low eccentricity
orbit with a semimajor axis of
23 AU.[6]
The first circumbinary extrasolar planet around a main sequence
star was found in 2005 in the system HD 202206: a Jupiter-size planet orbiting a
system composed of a Sun-like star and a brown dwarf.[7] A dynamical analysis of the
system further shows a 5:1 mean motion resonance between the planet and the
brown dwarf.[8] These observations raise the
question of how this system was formed, but numerical simulations show that a
planet formed in a circumbinary disk can migrate inward until it is captured in
resonance.[9]
Announced in 2008, the eclipsing binary system HW Virginis, comprising a subdwarf B star and a red dwarf, was announced to also host a
planetary system. The inner and outer planets have masses at least 8.47 and
19.23 times that of Jupiter respectively, and have orbital periods of 9 and 16
years. The outer planet is sufficiently massive that it may be considered to be
a brown dwarf under some definitions of the
term,[10] but the discoverers argue that
the orbital configuration implies it formed like a planet from a circumbinary
disc. Both planets may have accreted additional mass when the primary star lost
material during its red giant phase.[11]
On 15 September 2011, astronomers announced the first
partial-eclipse-based discovery of a circumbinary planet.[12][13] The planet, called Kepler-16b,
is about 200 light years from Earth, in the constellation Cygnus, and is
believed to be a frozen world of rock and gas, about the mass of Saturn. It
orbits two stars that are also circling each other, one about two-thirds the
size of our sun, the other about a fifth the size of our sun. Each orbit of the
stars by the planet takes 229 days, while the planet orbits the system's center
of mass every 225 days; the stars eclipse each other every three weeks or so.
Scientists made the finding through NASA's Kepler spacecraft, which launched in 2009 and
has been a driving force in the recent explosion in the discovery of distant
planets.
An artist's impression
of the binary star system HD 98800 B,
which is surrounded by a disc that may be in the process of forming planets.
HD 98800 B is itself a member of a quadruple star system.
Claims of a planet discovered via microlensing, orbiting the close binary
pair MACHO-1997-BLG-41,
were announced in 1999.[14] The planet was said to be in a
wide orbit around the twored dwarf companions,
but the claims were later retracted, as it turned out the detection could be
better explained by the orbital motion of the binary stars themselves.[15]
Several attempts have been made to detect planets around the
eclipsing binary system CM Draconis, itself
part of the triple system GJ 630.1. The eclipsing binary has been surveyed for
transiting planets, but no conclusive detections were made and eventually the
existence of all the candidate planets was ruled out.[16][17] More recently, efforts have
been made to detect variations in the timing of the eclipses of the stars
caused by the reflex motion associated with an orbiting planet, but at present
no discovery has been confirmed. The orbit of the binary stars is eccentric,
which is unexpected for such a close binary as tidal forces ought to have circularised
the orbit. This may indicate the presence of a massive planet or brown dwarf in orbit around the pair
whose gravitational effects maintain the eccentricity of the binary.[18]
Circumbinary discs that may indicate processes of planet formation
have been found around several stars, and are in fact common around binaries
with separations less than 3 AU.[19][20]One notable example is in the HD
98800 system, which comprises two pairs of binary stars separated by around 34
AU. The binary subsystem HD 98800 B, which consists of two stars of 0.70 and
0.58 solar masses in a highly eccentric orbit with semimajor axis 0.983 AU, is
surrounded by a complex dust disc that is being warped by the gravitational
effects of the mutually-inclined and eccentric stellar orbits.[21][22] The other binary subsystem, HD
98800 A, is not associated with significant amounts of dust.[23]
The Kepler results
indicate circumbinary planetary systems are relatively common (as of October
2013 the spacecraft had found seven planets out of roughly 1000 eclipsing binaries searched.
There is a wide range of stellar configurations for which
circumbinary planets can exist. Primary star masses range from 0.69 to 1.53solar masses (Kepler-16 A & PH1 Aa),
star mass ratios from 1.03 to 3.76 (Kepler-34 & PH1),
and binary eccentricity from 0.023 to 0.521 (Kepler-47 & Kepler-34). The distribution of planet
eccentricities, range from nearly circular e=0.007 to a significant e=0.182 (Kepler-16 &Kepler-34). No orbital resonances with the binary have
been found.[24]
The binary stars Kepler-34 A and B have a highly eccentric orbit
(e=0.521) around each other and their interaction with the planet is strong
enough that a deviation from Kepler's laws is noticeable after just
one orbit.[24]
All Kepler circumbinary planets that were known as of august 2013
orbit their stars very close to the plane of the binary (in a prograde
direction) which suggests a single-disk formation.[24] However not all circumbinary
planets are co-planar with the binary: Kepler-413b istilted 2.5
degrees which may be due to the gravitational influence of other planets or a
third star.[25][26]
The axial tilt of Kepler-413b's
spin axis might vary by as much as 30 degrees over 11 years, leading to rapid
and erratic changes in seasons.[26]
Simulations show that it is likely that all of the circumbinary
planets known prior to a 2014 study migrated significantly
from their formation location with the possible exception of Kepler-47(AB)c.[27]
The minimum stable star to circumbinary planet separation is about
2-4 times the binary star separation, or orbital period about 3-8 times the binary
period. The innermost planets in all the Kepler circumbinary systems have been
found orbiting close to this radius. The planets have semi-major axes that lie between 1.09 and
1.46 times this critical radius. The reason could be that migration might
become inefficient near the critical radius, leaving planets just outside this
radius.[24]
Most Kepler eclipsing binaries have periods less than 1 day but the
shortest period of a Kepler eclipsing binary hosting a planet is 7.4 days (Kepler-47). The short-period binaries are
unlikely to have formed in such a tight orbit and their lack of planets may be
related to the mechanism that removed angular momentum allowing the stars to
orbit so closely.[24]
As of August 2013 all the confirmed Kepler circumbinary planets
are smaller than Jupiter. This cannot be a selection effect because larger
planets are easier to detect.[24] Simulations had predicted this
would be the case.[28]
All the Kepler circumbinary planets are either close to or
actually in the habitable zone.
None of the them are terrestrial planets,
but largemoons of such planets could be habitable.
Because of the stellar binarity, the insolation received by the planet will
likely be time-varying in a way, quite unlike the regular sunlight Earth
receives.[24]
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