Can we believe in data of measurements?

[Weitter Duckss]

Full article at: Reassessment of the old but still employed theories of Universe through database checking

Can we believe in data of measurements

„Dysnomia, the moon of Eris, is beyond our abilities to acquire data in a credible way (that is obvious when talking about the less distant object of Haumea), but it should not be forgotten that nowadays scientists introduce, with "a high probability“, "relevant“ data for the exoplanets that are tens and thousands of light-years away. Therefore, the measurements are unreliable and should be treated as such, i.e., with caution. http://www.svemir-ipaksevrti.com/Universe-and-rotation.html#working-temperatures-of-elements

Size and mass of very large stars: Most massive example, VY Canis Majoris (17 ± 8 M_☉). Others are Rho Cassiopeiae (14-30 M_☉), Betelgeuse (11.6 ± 5.0 M_☉), and the blue Pistol Star (27.5 M_☉). The Sun (1 M_☉) Wikipedia

"A Beautiful Example" of Mathematics and Logic! Great mass has a small volume and vice versa. No wonder what about the density circulating fairy tale.

Type	Density [kg/m³]
Basalt magma	2650–2800
Andesite magma	2450–2500
Rhyolite magma	2180–2250

„Estimates of average density for the upper crust range between 2.69 and 2.74 g/cm³ and for lower crust between 3.0 and 3.25 g/cm³, Sun 1,408 g/cm³“^.  Wikipedia

Increasing temperature decreases the density.

Quotations from Wikipedie

White dwarfs resist gravitational collapse primarily through electron degeneracy pressure. (By comparison, main sequence stars resist collapse through thermal pressure.)

The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction. Consequently, white dwarfs with masses greater than the limit would be subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole. (However, white dwarfs generally avoid this fate by exploding before they undergo collapse.) Those with masses under the limit remain stable as white dwarfs.

-The currently accepted value of the limit is about 1.4 M_☉.

Sirius B

This mass is packed into a volume roughly equal to the Earth's (radius 0,0084 ± 3%   R _☉).  The current surface temperature is 25,200 K. Because there is no internal heat source, Sirius B will steadily cool as the remaining heat is radiated into space over more than two billion years.

A white dwarf forms only after the star has evolved from the main sequence and then passed through a red-giant stage. This occurred when Sirius B was less than half its current age, around 120 million years ago. The original star had an estimated 5 M_☉and was a B-type star (roughly B4–5) when it was still on the main sequence. While it passed through the red giant stage, Sirius B may have enriched the metallicity of its companion.

 Procyon B

With a surface temperature of 7,740 K, it is also much cooler than Sirius B; this is a testament to its lesser mass and greater age. The mass of the progenitor star for Procyon B was about 2.59+0.22−0.18 M_☉ and it came to the end of its life some 1.19±0.11 Gyr ago, after a main-sequence lifetime of 680±170 Myr.

Van Maanen 2

Like other white dwarfs, it is a very dense star: its mass has been estimated to be about 68% of the Sun's, yet it has only 1% of the Sun's radius. The outer atmosphere has a temperature of approximately 6,220 K, which is relatively cool for a white dwarf. As all white dwarfs steadily radiate away their heat over time, this temperature can be used to estimate its age, thought to be around 3 billion years.

The progenitor of this white dwarf had an estimated 2.6 solar masses and remained on the main sequence for about 9 × 10⁸ years. This gives the star a combined age of about 4.1 billion years. When this star left the main sequence, it expanded into a red giant that reached a maximum radius of 650 times the current radius of the Sun, or about 3 astronomical units

 L 97-12

The mass of L 97-12 is 0.59 ± 0.01 Solar masses, and its surface gravity is 10^{8.00 ± 0.02}cm·s⁻², or approximately 102,000 of Earth's, corresponding to a radius of 8,887 kilometres (5,522 miles), or 139% of Earth's.

L 97-12 has temperature 5,700 ± 90 K, almost like the Sun, and cooling age, i.e. age as degenerate star (not including lifetime as main-sequence star and as giant star) 2.65 ± 0.10 Gyr. Despite it is classified as "white dwarf", it should appear yellow, not white, nearly the same color as the Sun.

 LP 145-141

LP 145-141 has only 75% of the Sun's mass, but it is the remnant of a massive main-sequence star that had an estimated 4.4 solar masses. While it was on the main sequence, it probably was a spectral class B star (in the range B4-B9). Most of the star's original mass was shed after it passed into the asymptotic giant branch stage, just prior to becoming a white dwarf. 

 Wolf-Rayet star

The spectra indicate very high surface enhancement of heavy elements, depletion of hydrogen, and strong stellar winds. Their surface temperatures range from 30,000 K to around 200,000 K, hotter than almost all other stars.

 WR 2 

the exact rotation rate is not known. Estimates range from 500 km/s

 WR 46 

The effective temperature is over 110,000K, the luminosity greater than 600,000 times the solar luminosity (L_☉), the mass around 25 times that of the Sun (M_☉) and a radius of 2.9 times the solar radius (R_☉). The terminal velocity of the stellar wind reaches 2450 km/s

 WR 142

 Mass    20 M☉

Radius 0.40 R☉

Luminosity (bolometric)        245,000 L☉

Luminosity (visual, LV)         847  L☉

Temperature    200,000  K

Metallicity [Fe/H]       0.0  dex

Rotational velocity (v sin i)  1,000 km/s  

 WR

Mass    9.0 ± 0.6  M☉

Radius 6 ± 3  R☉

Luminosity (bolometric)        170,000  L☉

Temperature 57,000  K

Age     3.5-5.5 Myr

O

Mass    28.5 ±1.1 M☉

Radius 17 ± 2 R☉

Luminosity (bolometric)        280,000  L☉

Temperature    35,000  K

Age     3.5 -5.5  Myr

The brightest member, γ² Velorum or γ Velorum A, is a spectroscopic binary composed of a blue supergiant of spectral class O7.5 (~30 M_☉), and a massive Wolf-Rayet star (~9 M_☉, originally ~35 M_☉).  The binary has an orbital period of 78.5 days and separation varying from 0.8 to 1.6 astronomical units. 

 WR stars

Mass loss is influenced by a star's rotation rate, especially strongly at low metallicity. Fast rotation contributes to mixing of core fusion products through the rest of the star, enhancing surface abundances of heavy elements, and driving mass loss

 neutron star

As the star's core collapses, its rotation rate increases as a result of conservation of angular momentum, hence newly formed neutron stars rotate at up to several hundred times per second. Some neutron stars emit beams of electromagnetic radiation that make them detectable as pulsars.

 WOH G64

The combination of the star's temperature and luminosity places it toward the upper right corner of the Hertzsprung–Russell diagram. The star's evolved state means that it can no longer hold on to its atmosphere due to low density, high radiation pressure

 contrary to

 Gravitational collapse is the contraction of an astronomical object due to the influence of its own gravity, which tends to draw matter inward toward the center of mass. Gravitational collapse is a fundamental mechanism for structure formation in the universe. Over time an initial, relatively smooth distribution of matter will collapse to form pockets of higher density, typically creating a hierarchy of condensed structures such as clusters of galaxies, stellar groups, stars and planets.

Etc.