The study and
analysis of Super Massive Black Holes (SMBH) is of interest to determine
characteristics in the Primordial Universe where matter had an enormous
density, similar or higher than that of Neutron Stars.
But finding this
type of SMBH objects in the form of quasars (with high redshift) far away, or
in Active Galactic Nuclei (AGN) as in the center of our Milky Way, poses
serious limitations that have to do with existing science and technology.
An alternative
already mentioned in other posts by me, is the study of primordial Neutron
Stars (NS). If SMBH could be formed without going through Population III stars
(Pop III) that are that type of low metallicity stars (the first to form). Then
there may also be primordial NS. The problem is detecting these objects.
One way to
detect a "very cold" NS (just as a White Dwarf has a Debye-cooling
regime thermal equilibrium process), would be to find it with an M Dwarf
companion. The "red dwarfs" are stars (Pop III), which due to their
size and low radiative emission can have a life equal to or greater than that
of our universe. The M Dwarf that we look for in a Multiple Star System is in a
group called Ultra poor mentality (UPM).
At present, the
M Dwarfs have become objects of high interest for science, since they can be
accompanied by other stars such as Multiple Star Systems or Exoplanets. And as
I mention in this article there are multiple programs and observatories looking
for them.
Discovered
systems that are interesting.
Binary system. A
colder NS with a partner (WD or NS) encountered radio telescopes. doi: 10.1088
/ 0004-637X / 789/2/119
We also have the
fusion of two massive objects that no visual remnant was found. The fusion of a
23 solar mass BH Object and a 2.6 solar mass companion (NS or BH). arXiv:
2006.12611v1
The
characteristics of the M-Dwarf that interest me are: Ultra poor mentality
(UPM). Of which there is an interesting list. arXiv: 1603.08040v2; doi: 10.1088
/ 0004-637X / 745/2/118; doi: 10.1088 / 0004-6256 / 140/3/844.
Strategy: NS-M
Dwarf detection and observation method.
In this case,
Radial Velocity should be the main method (to rule out that the companion of an
M Dwarf is of lower mass, we look for a very cold NS).
1) Various
astrometric and photometric methods.
2) Radial
velocity.
3) Astrometry.
4) Transit Time
Variation (Transit Timing Varations, TTV).
5) Press Timing,
PT.
Observation /
Programs:
|
Chandra RX. eRosita RX. GAIA. Hubble Visible. XMM Newton. NICER RX (Pulsar’s). TESS. NGTS. ASPERA. KEPLER/2. |
Keck Observatory NIR. Subaru NIR. VLBI. CRIRES: cryogenic high-resolution infrared echelle spectrograph for
the VLT Telescope Carlos Sánchez (TCS), MuSCAT2. ALMA. STARE. The WASP Project and the SuperWASP Cameras – JSTOR. LIGO Livingston, LIGO
Hanford y Virgo. Telescopios Magallanes -
Las Campanas Observator. ALMA. STARE. |
Note: In the
future JWST, GMT, ELT, TMT telescope, Roman Telescope and mini space telescopes
...
LAMOST and
eROSITA
We have two very
special tech programs to mention in M Dwarf's research.
LAMOST.
M-dwarf stars are the most common stars in the galaxy and dominate the galaxy's
population at weak magnitudes. Precise and exact stellar parameters for M
dwarfs are of crucial importance for many studies. However, the atmospheric
parameters of M dwarf stars are difficult to determine. In this article, we
present a catalog of the spectroscopic stellar parameters (Teff and [M / H]) of
∼300,000 M dwarf
stars observed by both LAMOST and Gaia using the Stellar LAbel Machine (SLAM).
We trained a SLAM model using LAMOST spectra with APOGEE Data Release 16 tags
with 2800 K <Teff <4500K and −2 dex <[M / H] <0.5 dex. The SLAM
Teff agrees within 50 K compared to the previous study determined by the APOGEE
observations, and the SLAM [M / H] agrees within 0.12 dex compared to the
APOGEE observation. We also established a SLAM model trained by the BT-Settl
atmospheric model with random uncertainties (in cross validation) at 60 K and
agreeing within ∼90 K
compared to previous studies.
LAMOST
https://doi.org/10.3847/1538-4365/abe1c1
eROSITA
(Extended ROentgen Study with an Imaging Telescope Array) is the main
instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission. eROSITA is
currently being built, assembled and tested under the leadership of the
Max-Planck Institute for Extraterrestrial Physics (MPE). In the first four
years of scientific operation after launch, eROSITA will perform an in-depth
survey of the entire X-ray sky. In the soft X-ray band (0.5-2 keV), this will
be approximately 20 times more sensitive than sounding ROSAT all sky, while in
the hard band (2-10 keV) will provide the first true imaging study of the sky
with those energies. Such a sensitive survey of the whole sky will revolutionize
our view of the high-energy sky, and demands great efforts in synergistic,
multi-wavelength wide-area studies in order to take full advantage of the
scientific potential of X-ray data. The Whole Sky Survey The program will be
followed by an estimated 3.5 years of spot observations, with open access
through regular announcement of opportunities for the entire astrophysics’
community. With on-axis resolution similar to that of XMM-Newton, a comparable
effective area at low energies and a field of view, eROSITA will provide a
powerful and highly competitive X-ray observatory for the next decade.
NS detection
• Most are
pulsars.
• Cold NS.
• NS without
companion, emission detected by radio telescopes or RX telescopes and possibly
gamma.
• Accompanied
NS, binary or three-component system. Ideally, it would not interact with the
partners absorbing mass (that will raise the temperature).
• DW-NS or
M-Dwarf-NS network; Blue dim Dwarf-NS (No stars are known in the post-red dwarf
stage). Low in Metallicity, possibly low mass, cold.
