WilloWISPs: A New Dark Growth Channel for Black Holes Suggests a Full-Spectrum Hierarchical MACHO Mass Function for Dark Matter (2502.06981v2)

Abstract: Evidence of neutron stars with deconfined quark-matter cores suggest a new pathway for the evolution of black holes. New theories about the cores of neutron stars support the idea that quarkonium is likely to grow there as the neutron star ages. Surveys of stellar remnants have shown that there is no major mass gap between neutron stars and black holes. Black holes, specifically primordial ones (PBHs), have been suggested as an explanation for dark matter before. However, the way that very large black holes can form in the lifetime of the visible universe has only recently been explained with a promising solution to The Final Parsec Problem. If neutron stars can become exotic stars or black holes surrounded by axions, then they may allow Intermediate-Mass Black Holes (IMBH) and Supermassive Black Holes (SMBH) to form quickly enough via coalescence. We find that a hierarchical clustering of Massive and Compact Halo Objects (MACHOs) with axion-dominated mini-halos can help to explain all of the missing dark matter. The model presented here suggests that this type of MACHO is likely equivalent to black holes above an unknown critical mass, which is less than ~1 $M_{\odot}$, and that they ought to be quark stars below this mass. If quark stars are a transition state between neutron stars and black holes, then black holes ought to be equivalent to boson stars, after all the residual quark material has formed a Bose-Einstein condensate of strange mesons.

• The paper introduces a novel MACHO mass function where WilloWISPs drive black hole growth via dark matter interactions.
• It demonstrates neutron star evolution transitioning to quark stars, bridging the gap to intermediate and supermassive black holes.
• It proposes gravitational detection methods, such as observing axion-induced gasers, to validate the model of dark matter and black hole interplay.

Analysis of "WilloWISPs: A New Dark Growth Channel for Black Holes"

The theoretical paper by Smith and Comins explores a novel concept in astrophysical research concerning the evolution of certain celestial phenomena, particularly the role of Massive and Compact Halo Objects (MACHOs) in the dark matter narrative. The paper suggests a refined model for black hole and dark matter interaction, positing that structures termed "WilloWISPs" might provide critical insights into the missing components of dark matter.

The investigation centers on the evolution of neutron stars that could potentially metamorphose into quark stars or exotic stars, eventually leading to the formation of black holes. The paper leverages observations indicating no significant mass gap between neutron stars and black holes, bolstered by the hypothesis that neutron stars are capable of transitioning into quark stars with quarkonium cores. These transitions might significantly contribute to the creation and mass accumulation of Intermediate-Mass Black Holes (IMBHs) and Supermassive Black Holes (SMBHs), challenging traditional views on dark matter composition.

Key Findings and Theoretical Implications

1. Dark Matter and Black Hole Growth: The authors present a MACHO mass function, proposing that dark matter could indeed be comprehensively represented by a spectrum of black holes and non-trivial celestial objects. Essential to this framework is the idea that dark matter density spikes, or Ultra-Compact Mini Halos (UCMHs), which are enriched with axions rather than Weakly Interacting Massive Particles (WIMPs), could accelerate the growth of nearby stellar structures into black holes.
2. Neutron Star Evolution: The implications for neutron star evolution are significant. The transition from neutron stars into other forms like quark stars, possibly mediated by deconfined quark-matter cores, suggests that such objects might be more widespread than previously assumed, representing a substantial reservoir for dark matter.
3. Gravitational Dynamics and Accretion: The research introduces the concept of quark drip and gravitational influences that could support the condensation of quark material within these stars. Such dynamics have practical implications for understanding how accretion events and gravitational imaging could reveal hidden aspects of cosmic dark matter.
4. WilloWISPs as Dark Matter Candidates: The model unveils "WilloWISPs" as potential candidates for dark matter. These represent a fusion of black holes with axion clouds forming UCMHs. The paper positions these compositions as capable of explaining nearly all missing dark matter, owing to their propensity for forming through the evolution of neutron stars into quark stars and then into black holes.
5. Detection Methods: The discussion on gravitational-lasers or "gasers" caused by axions around black holes is crucial, suggesting that with instruments like LISA, the paper of gravitational radiation could extend our understanding of axion roles in these processes.

Contributions to Dark Matter Theories and Future Prospects

Smith and Comins' exploration narrows the focus on axion-rich environments in dark matter halos, positioning these in the WilloWISP model as a potential unifying theory for dark matter. This formulation challenges the conventional understanding by exploring non-standard stellar evolutionary paths, uncovering new avenues for black hole and dark matter interaction.

Future investigations that probes the details of quark matter configurations within black holes and neutron star cores, along with further observational campaigns targeting axion effects and MACHO distributions, are encouraged. This could entail observational support using advanced instruments ready to detect signals consistent with these new theoretical predictions. Additionally, refining the equations of state for quarkonium could deeply enhance the comprehension of the quantum chromodynamics that underpin these massive astrophysical phenomena.

Ultimately, this work grants profound insight into the complexities of dark matter, expanding the framework within which we understand the interaction between stellar remnants, dark matter, and cosmic structure formation processes.