Mg II h + k Flux—Rotational Period Correlation for G-type Stars

Manuel Olmedo, Miguel Chávez, Emanuele Bertone, Víctor De la Luz

Research output: Contribution to journalArticle

Abstract

We present an analysis of the correlation between the mid-UV Mg II h and k emission lines and measured rotational periods of G-type stars. Based on IUE and HST high resolution spectra of a sample of 36 stars, we derive an exponential function that best represents the correlation. We found that the variation of the Mg II h + k fluxes is about a factor of 2.5 larger than that of Ca II H+K, indicating that the UV features are more sensitive to the decline of rotational period. The comparison of UV-predicted rotational periods with those derived from empirical Prot - Ca II H+K flux calibrations are consistent, with some scatter at large periods, where the emission are less intense. We present newly derived rotational periods for 15 G-type stars.
Original languageEnglish
Pages (from-to)1436
JournalPublications of the Astronomical Society of the Pacific
Volume125
Issue number934
DOIs
Publication statusPublished - 1 Dec 2013
Externally publishedYes

Fingerprint

stars
IUE
exponential functions
calibration
high resolution
comparison
analysis

Cite this

Olmedo, Manuel ; Chávez, Miguel ; Bertone, Emanuele ; De la Luz, Víctor. / Mg II h + k Flux—Rotational Period Correlation for G-type Stars. In: Publications of the Astronomical Society of the Pacific. 2013 ; Vol. 125, No. 934. pp. 1436.
@article{3c67c8faed7949b686363d08090bbe00,
title = "Mg II h + k Flux—Rotational Period Correlation for G-type Stars",
abstract = "We present an analysis of the correlation between the mid-UV Mg II h and k emission lines and measured rotational periods of G-type stars. Based on IUE and HST high resolution spectra of a sample of 36 stars, we derive an exponential function that best represents the correlation. We found that the variation of the Mg II h + k fluxes is about a factor of 2.5 larger than that of Ca II H+K, indicating that the UV features are more sensitive to the decline of rotational period. The comparison of UV-predicted rotational periods with those derived from empirical Prot - Ca II H+K flux calibrations are consistent, with some scatter at large periods, where the emission are less intense. We present newly derived rotational periods for 15 G-type stars.",
author = "Manuel Olmedo and Miguel Ch{\'a}vez and Emanuele Bertone and {De la Luz}, V{\'i}ctor",
year = "2013",
month = "12",
day = "1",
doi = "10.1086/674332",
language = "English",
volume = "125",
pages = "1436",
journal = "Publications of the Astronomical Society of the Pacific",
issn = "0004-6280",
publisher = "University of Chicago",
number = "934",

}

Mg II h + k Flux—Rotational Period Correlation for G-type Stars. / Olmedo, Manuel; Chávez, Miguel; Bertone, Emanuele; De la Luz, Víctor.

In: Publications of the Astronomical Society of the Pacific, Vol. 125, No. 934, 01.12.2013, p. 1436.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Mg II h + k Flux—Rotational Period Correlation for G-type Stars

AU - Olmedo, Manuel

AU - Chávez, Miguel

AU - Bertone, Emanuele

AU - De la Luz, Víctor

PY - 2013/12/1

Y1 - 2013/12/1

N2 - We present an analysis of the correlation between the mid-UV Mg II h and k emission lines and measured rotational periods of G-type stars. Based on IUE and HST high resolution spectra of a sample of 36 stars, we derive an exponential function that best represents the correlation. We found that the variation of the Mg II h + k fluxes is about a factor of 2.5 larger than that of Ca II H+K, indicating that the UV features are more sensitive to the decline of rotational period. The comparison of UV-predicted rotational periods with those derived from empirical Prot - Ca II H+K flux calibrations are consistent, with some scatter at large periods, where the emission are less intense. We present newly derived rotational periods for 15 G-type stars.

AB - We present an analysis of the correlation between the mid-UV Mg II h and k emission lines and measured rotational periods of G-type stars. Based on IUE and HST high resolution spectra of a sample of 36 stars, we derive an exponential function that best represents the correlation. We found that the variation of the Mg II h + k fluxes is about a factor of 2.5 larger than that of Ca II H+K, indicating that the UV features are more sensitive to the decline of rotational period. The comparison of UV-predicted rotational periods with those derived from empirical Prot - Ca II H+K flux calibrations are consistent, with some scatter at large periods, where the emission are less intense. We present newly derived rotational periods for 15 G-type stars.

U2 - 10.1086/674332

DO - 10.1086/674332

M3 - Article

VL - 125

SP - 1436

JO - Publications of the Astronomical Society of the Pacific

JF - Publications of the Astronomical Society of the Pacific

SN - 0004-6280

IS - 934

ER -