RED LIGHTHOUSE

 

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.