Skip to content
DraconiticResearch
Search Sources API
203,203 studies31 sourcesUpdated 23 min ago
PreprintCC BY 4.0arXiv

Predicting Macroturbulence in F/G/K Dwarfs to 100 m/s Precision

  • Jack Lubin
  • Erik Petigura
  • Kento Masuda
  • Samuel Halverson
  • Isabel Angelo
  • Daniel Huber
  • Michael L. Palumbo III
  • Songhu Wang
  • Xian-Yu Wang
Open at sourcePDFDOICite

Abstract

We leverage the high resolution and spectral stability of the Keck Planet Finder (KPF) spectrograph to investigate macroturbulence broadening via the stellar cross-correlation function (CCF). As our calibration sample, we use main sequence benchmark slow-rotators vsini < 4 km/s where rotation rates were derived from the most robust asteroseismic mode splitting measurements, independent from spectral line broadening. We fit a linear relationship for macroturbulence as a function of derived νmax, the frequency of maximum power due to stellar oscillations, with an RMS scatter of 90 m/s. Previous studies have calibrated macroturbulence against Teff, but we find νmax to be a lower dispersion predictor by a factor of 4 indicating a deeper relationship between νmaxand convective motions.

Related

  1. Astrometric planet search around southern ultracool dwarfs. V. Discovery of the exoplanet candidate PALTA-1 b
    J. Sahlmann, P. F. Lazorenko, E. L. Martín +3
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref
  2. Radial velocity follow-up of astrometric substellar companions: 6 confirmed brown dwarfs and 13 impostor binaries Gaia
    Marcus L. Marcussen, Simon H. Albrecht, Kamil K. Kalinowski +7
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref
  3. Euclid Early Release Observations of the Barnard 30 dark cloud I. Brown dwarfs and planetary mass candidate members at the core of the association
    D Barrado, H Bouy, E.L Martin +8
    HALPreprintLicence not statedGeneral astronomyGeneral physicsHAL
  4. Chromospheric fluxes from the Ca II infrared triplet in M dwarfs. A homogeneous catalog from CARMENES spectra
    P. V. Souza dos Santos, H. M. Tabernero, I. Ribas +10
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref
  5. EPRV asteroseismology of the K dwarfs GJ 570 A and GJ 783 A with ESPRESSO. Empirical mode-amplitude scaling in tension with 3D convection simulations
    T. L. Campante, Y. Zhou, Y. Li +21
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref

Cite

BibTeXRIS
BibTeX
@misc{lubin2026predicting,
  title = {{Predicting Macroturbulence in F/G/K Dwarfs to 100 m/s Precision}},
  author = {Jack Lubin and Erik Petigura and Kento Masuda and Samuel Halverson and Isabel Angelo and Daniel Huber and Michael L. Palumbo III and Songhu Wang and Xian-Yu Wang},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.17693},
  eprint = {2609.17693},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.17693},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Predicting Macroturbulence in F/G/K Dwarfs to 100 m/s Precision
AU  - Jack Lubin
AU  - Erik Petigura
AU  - Kento Masuda
AU  - Samuel Halverson
AU  - Isabel Angelo
AU  - Daniel Huber
AU  - Michael L. Palumbo III
AU  - Songhu Wang
AU  - Xian-Yu Wang
PY  - 2026
DA  - 2026/09/15
PB  - arXiv
DO  - 10.48550/arxiv.2609.17693
UR  - https://arxiv.org/abs/2609.17693
AB  - We leverage the high resolution and spectral stability of the Keck Planet Finder (KPF) spectrograph to investigate macroturbulence broadening via the stellar cross-correlation function (CCF). As our calibration sample, we use main sequence benchmark slow-rotators vsini < 4 km/s where rotation rates were derived from the most robust asteroseismic mode splitting measurements, independent from spectral line broadening. We fit a linear relationship for macroturbulence as a function of derived ν_max, the frequency of maximum power due to stellar oscillations, with an RMS scatter of 90 m/s. Previous studies have calibrated macroturbulence against T_eff, but we find ν_max to be a lower dispersion predictor by a factor of 4 indicating a deeper relationship between ν_maxand convective motions.
ER  -