# On Star 5-Colorings of Sparse Graphs

**Authors:** Ilkyoo Choi, Boram Park

arXiv: 1903.10133 · 2019-09-26

## TL;DR

This paper improves bounds on the star chromatic number of sparse graphs, showing that graphs with maximum average degree at most 8/3 have a star 5-coloring, and applies this to planar graphs with high girth.

## Contribution

It establishes tighter bounds on star colorings for sparse graphs, notably proving that max average degree ≤ 8/3 guarantees a star 5-coloring, and improves girth conditions for planar graphs.

## Key findings

- Graphs with mad(G) ≤ 8/3 have star chromatic number at most 5.
- Planar graphs with girth at least 8 are star 5-colorable.
- Improved previous bounds on star colorings of sparse graphs.

## Abstract

A \textit{star $k$-coloring} of a graph $G$ is a proper (vertex) $k$-coloring of $G$ such that the vertices on a path of length three receive at least three colors. Given a graph $G$, its \textit{star chromatic number}, denoted $\chi_s(G)$, is the minimum integer $k$ for which $G$ admits a star $k$-coloring. Studying star coloring of sparse graphs is an active area of research, especially in terms of the maximum average degree of a graph; the \textit{maximum average degree}, denoted $mad(G)$, of a graph $G$ is $\max\left\{ \frac{2|E(H)|}{|V(H)|}:{H \subset G}\right\}$. It is known that for a graph $G$, if $mad(G)<\frac{8}{3}$, then $\chi_s(G)\leq 6$, and if $mad(G)< \frac{18}{7}$ and its girth is at least 6, then $\chi_s(G)\le 5$. We improve both results by showing that for a graph $G$, if $mad(G)\le \frac{8}{3}$, then $\chi_s(G)\le 5$. As an immediate corollary, we obtain that a planar graph with girth at least 8 has a star 5-coloring, improving the best known girth condition for a planar graph to have a star 5-coloring.

## Full text

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## Figures

18 figures with captions in the complete paper: https://tomesphere.com/paper/1903.10133/full.md

## References

21 references — full list in the complete paper: https://tomesphere.com/paper/1903.10133/full.md

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Source: https://tomesphere.com/paper/1903.10133