scholarly journals Age Determinations of Early-M Type Pre-Main Sequence Stars Using a High-Resolution Near-Infrared Spectroscopic Method

2011 ◽  
Vol 63 (3) ◽  
pp. 677-684 ◽  
Author(s):  
Yuhei Takagi ◽  
Yoichi Itoh ◽  
Yumiko Oasa ◽  
Koji Sugitani
Keyword(s):  
High Resolution ◽  
Main Sequence ◽  
Near Infrared ◽  
Spectroscopic Method ◽  
Main Sequence Stars ◽  
Infrared Spectroscopic ◽  
Age Determinations

scholarly journals IN-SYNC I: HOMOGENEOUS STELLAR PARAMETERS FROM HIGH-RESOLUTION APOGEE SPECTRA FOR THOUSANDS OF PRE-MAIN SEQUENCE STARS

2014 ◽  
Vol 794 (2) ◽  
pp. 125 ◽  
Author(s):  
Michiel Cottaar ◽  
Kevin R. Covey ◽  
Michael R. Meyer ◽  
David L. Nidever ◽  
Keivan G. Stassun ◽  
...  
Keyword(s):  
High Resolution ◽  
Main Sequence ◽  
Main Sequence Stars

Method transfer of a near-infrared spectroscopic method for blend uniformity in a poorly flowing and hygroscopic blend

2020 ◽  
Vol 180 ◽  
pp. 113054 ◽  
Author(s):  
Bárbara B. Alvarado-Hernández ◽  
James V. Scicolone ◽  
Carlos Ortega-Zuniga ◽  
Andrés D. Román-Ospino ◽  
Yleana M. Colón-Lugo ◽  
...  
Keyword(s):  
Near Infrared ◽  
Spectroscopic Method ◽  
Method Transfer ◽  
Blend Uniformity ◽  
Infrared Spectroscopic

A Discussion on astronomy in the ultraviolet - The ultraviolet spectrum of B-type supergiants

1975 ◽  
Vol 279 (1289) ◽  
pp. 429-442
Keyword(s):  
High Resolution ◽  
Spectral Type ◽  
Main Sequence ◽  
Ultraviolet Spectrum ◽  
Absorption Lines ◽  
Light Elements ◽  
Main Sequence Stars ◽  
Complete Identification ◽  
Constant Strength

The broad, steep-sided absorption lines in B-type supergiant spectra are stronger than the absorption lines in main-sequence stars. In addition to lines from the second, third and fourth spectra of the light elements and the metals there is a broad, pointed feature at 1720 A which has constant strength in the B-type supergiants regardless of spectral type. The complete identification of this blend is not known. At high resolution the ultraviolet resonance lines of C iv, N v, Si hi and Si iv in the spectra of OB supergiants are shortward displaced by velocities up to 1800 km s-1 indicating the presence of an escaping atmosphere. At type B5 the expanding atmosphere is moving at about 120 km s-1 which means that the material is probably brought to rest before it escapes from the star. Evidence is presented of the presence of a stationary shell around the B5Ia supergiant q Canis Majoris as well as a slowly expanding atmosphere.

Applicability of Near-infrared Spectroscopic Method to Unfreezable Water Measurements in Egg White Lysozyme and Soluble Starch

LWT ◽  
1997 ◽  
Vol 30 (4) ◽  
pp. 406-410 ◽  
Author(s):  
Jin-hwan Hong ◽  
Sakiyo Yamaoka-Koseki ◽  
Yoshinobu Tsujii ◽  
Kyoden Yasumoto
Keyword(s):  
Near Infrared ◽  
Spectroscopic Method ◽  
Soluble Starch ◽  
Egg White ◽  
Egg White Lysozyme ◽  
Infrared Spectroscopic ◽  
Unfreezable Water

EXPANDING THE CHARA/FLUOR HOT DISKS SURVEY

2013 ◽  
Vol 02 (02) ◽  
pp. 1340010 ◽  
Author(s):  
B. MENNESSON ◽  
N. SCOTT ◽  
T. TEN BRUMMELAAR ◽  
G. BRYDEN ◽  
N. TURNER ◽  
...  
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Near Infrared ◽  
Dust Cloud ◽  
Main Sequence Stars ◽  
Second Development ◽  
Zodiacal Dust ◽  
Dust Component ◽  
Initial Survey ◽  
Better Than

Little is presently known about the hot (>300 K) dust component of debris disks surrounding main sequence stars, similar to the zodiacal dust cloud found in the inner solar system. While extensive surveys have been carried out from space, the majority of detections have surprisingly come from the ground, where near infrared interferometric observations have recently revealed small (~1%) resolved excesses around a dozen nearby main sequence stars. Most of these results have come from the CHARA array "FLUOR" instrument (Mt. Wilson, CA), which has demonstrated the best sensitivity worldwide so far for this type of studies, and has carried out an initial survey of ~40 stars. In order to further understand the origin of this "hot dust phenomenon", we will extend this initial survey to a larger number of stars and lower excess detection limits, i.e. higher visibility accuracy providing higher contrast measurements. To this end, two major instrumental developments are underway at CHARA. The first one aims at improving FLUOR's sensitivity to a median K-band magnitude limit of 5 (making 200 targets available). The second development is based on a method that we recently developed for accurate (better than 0.1%) null depth measurements of stars, and that can be extended to regular interferometric visibility measurements.

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