We present an analysis of the chemical abundances and kinematics of six low-mass dwarf stars, previously claimed to be candidate hypervelocity stars (HVSs). We obtained moderate-resolution ($R\sim6000$) spectra of these stars to estimate the abundances of several chemical elements (Mg, Si, Ca, Ti, Cr, Fe, and Ni), and derived their space velocities and orbital parameters using proper motions from the \gaia\ Data Release 2. All six stars are shown to be bound to the Milky Way, and in fact are not even considered high-velocity stars with respect to the Galactic rest frame. Nevertheless, we attempt to characterize their parent Galactic stellar components by simultaneously comparing their element abundance patterns and orbital parameters with those expected from various Galactic stellar components. We find that two of our program stars are typical disk stars. For four stars, even though their kinematic probabilistic membership assignment suggests membership in the Galactic disk, based on their distinct orbit l properties and chemical characteristics, we cannot rule out exotic origins as follows. Two stars may be runaway stars from the Galactic disk. One star has possibly been accreted from a disrupted dwarf galaxy or dynamically heated from a birthplace in the Galactic bulge. The last object may be either a runaway disk star or has been dynamically heated. Spectroscopic follow-up observations with higher resolution for these curious objects will provide a better understanding of their origin.

Abstract
1. INTRODUCTION
2. SPECTROSCOPIC OBSERVATIONS AND REDUCTION
3. ESTIMATION OF STELLAR PARAMETERS ANDCHEMICAL ABUNDANCES
4. KINEMATIC AND CHEMICAL PROPERTIES OF OURPROGRAM STARS
    4.1. Kinematic Properties
    4.2. Chemical Properties
5. DISCUSSION
    5.1. SDSS J113102.87+665751.1 (Pal14 ID 4)
    5.2. SDSS J064337.13+291410.0 (Pal14 ID 7)
    5.3. SDSS J172630.60+075544.0 (Pal14 ID 10)
    5.4. SDSS J095816.39+005224.4 (Pal14 ID 15)
    5.5. SDSS J074728.84+185520.4 (Pal ID 16)
    5.6. SDSS J064257.02+371604.2 (Pal ID 17)
6. SUMMARY AND CONCLUSIONS
REFERENCES

• Bum-Suk Yeom(Department of Astronomy and Space Science, Chungnam National University/Jeollabukdo Institute of Science Education)
• Young Sun Lee(Department of Astronomy and Space Science, Chungnam National University) Corresponding author
• Jae-Rim Koo(Department of Astronomy and Space Science, Chungnam National University)
• Timothy C. Beers(Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame)
• Young Kwang Kim(Department of Astronomy and Space Science, Chungnam National University)