Orodruin said:
No, I think your interpretation of it is wrong. It is talking about the large scale structure formation, not about structures made of neutrinos.
Perhaps I'm misuing the word "structure". Let's see if I can clarify what I mean...
I don't necessarily mean compact structures like a "neutrino star", but more like diffuse halos surrounding large scale structures (I asked about halos surrounding galaxies before, but it's true that if we are considering large scale structures, we should be rather talking about
clusters of galaxies).
For example, in the OP I linked a similar question to my own (
https://physics.stackexchange.com/questions/80390/are-neutrino-stars-theoretically-possible). The most voted answer proposes that rather than "neutrino stars", there could be "halos of degenerate neutrino gas around galactic clusters" and it links to this other paper (
https://academic.oup.com/mnras/article/434/3/2679/1046015) which discusses the possibility of the presence of neutrino halos around large scale structures. In the introduction, it indicates:
The Λ cold dark matter (ΛCDM) paradigm has been embraced after it was realized that the most natural DM candidate, the neutrino, seems incapable to explain the formation of large-scale structures such as galaxies and galaxy clusters. ΛCDM has been successful in describing the cosmic microwave background and large-scale structures. It is adaptable to many other situations, though often not predictive. However, despite decades and dozens of searches, the CDM particle has not been established (Aprile et al. 2012), also not at the Large Hadron Collider (Aad et al. 2011), so one may wish to keep an open eye at other scenarios.
It has been put forward by Gibson (1996) that in the early Universe the role of turbulence and viscosity in the protoplasma and after the transition to neutral gas is more important than commonly assumed. Gravitational hydrodynamics alone is capable to explain large-scale structure formation without CDM trigger, in a three-step top-down scenario; see also Nieuwenhuizen, Gibson & Schild (2009). First, the plasma undergoes a viscous fragmentation at redshift z = 5100, creating voids of 40 Mpc comoving size. After the decoupling of photons the gas condenses in Jeans clumps of 600 000 solar masses and they in their turn fragment in 200 billion micro brown dwarfs of Earth weight. This picture explains a wealth of observations (Schild 1996; Nieuwenhuizen et al. 2009; Nieuwenhuizen, van Heusen & Liska 2012) and motivates to re-open our minds for the possibility of free-streaming DM, like neutrino hot DM.
Which apparently indicates that there could be halos formed by light neutrinos with high speeds* (which I guess that could increase in size as neutrinos lose kinetic energy over time, but please correct me if I'm wrong on this)
And in this paper (
https://arxiv.org/pdf/astro-ph/9707285), in section 1.7.6. the author proposes that mixed dark matter models (with both cold and hot dark matter) do explain better our observations as we would need less-clustered dark matter to address them concerning large scale structure formation. It specifically mentions simulations of extended hot dark matter halos.
Also here (
https://franciscovillaescusa.github.io/neutrinos.html) the author shows some simulations of halos of light neutrinos that become more aggregated once their speed becomes low enough and compares it with cold dark matter.
Considering all of this, couldn't these types of "structures" (If the word "structures" is the right term) of light neutrino halos be physically possible (even more, when the neutrinos will lose kinetic energy with time)? I mean, couldn't there be diffuse and less clustered groups of matter consisting of standard model neutrinos that would become a bit more clustered as they lose kinetic energy over time?
Or even in that case all of this is wrong and no such structures could possibly ever form? Then why do these authors even mention hot dark matter halos as a possibility?
*please note that the author talks about models of free streaming neutrinos (or hot dark matter), but here (
https://adlibitum.oats.inaf.it/seminari/nieuwenhuizen.pdf) he nuances that they are free streaming up until being trapped by a galaxy cluster