# Self-Gravitating Bose-Einstein Condensates and the Thomas-Fermi Approximation

## Abstract

**:**

## 1. Introduction

## 2. Discussion

## 3. Conclusions

## Acknowledgments

## Conflicts of Interest

## References

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**Figure 2.**Density cross-section of a stable simulated $1\phantom{\rule{3.33333pt}{0ex}}{M}_{\odot}$, $r\simeq 50$ km Bose-star (or stellar core) after approximately 300,000 numerical iterations that corresponds to 3 s [21]. (For comparison, the period of a circular orbit at $r=50$ km is approximately 0.006 s.) Axes are in km, density is in units of ${10}^{30}\phantom{\rule{3.33333pt}{0ex}}\mathrm{kg}/{\mathrm{km}}^{3}\simeq 0.5\phantom{\rule{3.33333pt}{0ex}}{M}_{\odot}/{\mathrm{km}}^{3}$. NB: The spatial grid used in this simulation is low resolution ($60\times 60\times 60$) and image smoothing was used to improve the presentation quality.

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Toth, V.T. Self-Gravitating Bose-Einstein Condensates and the Thomas-Fermi Approximation. *Galaxies* **2016**, *4*, 9.
https://doi.org/10.3390/galaxies4030009

**AMA Style**

Toth VT. Self-Gravitating Bose-Einstein Condensates and the Thomas-Fermi Approximation. *Galaxies*. 2016; 4(3):9.
https://doi.org/10.3390/galaxies4030009

**Chicago/Turabian Style**

Toth, Viktor T. 2016. "Self-Gravitating Bose-Einstein Condensates and the Thomas-Fermi Approximation" *Galaxies* 4, no. 3: 9.
https://doi.org/10.3390/galaxies4030009