A New Look at the HS Hydrae System

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10455234" target="_blank" >RIV/00216208:11320/22:10455234 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=S3mvxrhtpw" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=S3mvxrhtpw</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/ac4492" target="_blank" >10.3847/1538-3881/ac4492</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A New Look at the HS Hydrae System

Popis výsledku v původním jazyce

A growing group of stellar triple systems contains an eclipsing binary for which the depth of eclipses has been proven to change in time, a sign of evolving orbital inclination. The recent analysis of historical observations of HS Hya significantly extended the timespan over which the inclination changes are known for this system. Here we add a few more observations and reanalyze the whole data set with a single methodology. We also improve our own analytical approach to enable describing the secular evolution of the orbital architecture of hierarchical triple systems applicable to the HS Hya case. Analyzing the available photometric and spectroscopic data we obtain two main results. First, the dynamical evolution itself allows to constrain the masses of the stars in the inner binary to 1.31 +/- 0.03 M-circle dot and 1.27 +/- 0.03 M-circle dot, and the mass of the unseen third component to 0.56(-0.09)(+0.12)M(circle dot) (all 95% confidence level results). This makes it an M- or K-type dwarf accompanying the binary. Second, the orbital planes of the inner binary and the third component are significantly noncoplanar, allowing two solutions for their mutual angle J. Either the motion of the third component is prograde, and J is most likely in the 50 degrees -65 degrees range, or the motion is retrograde, and J is most likely in the 120 degrees -150 degrees range. The precession period of both orbital planes about the total angular angular momentum is similar to 700 yr (with about two centuries of uncertainty). This implies HS Hya will become eclipsing again around the year 2200.

Název v anglickém jazyce

A New Look at the HS Hydrae System

Popis výsledku anglicky

A growing group of stellar triple systems contains an eclipsing binary for which the depth of eclipses has been proven to change in time, a sign of evolving orbital inclination. The recent analysis of historical observations of HS Hya significantly extended the timespan over which the inclination changes are known for this system. Here we add a few more observations and reanalyze the whole data set with a single methodology. We also improve our own analytical approach to enable describing the secular evolution of the orbital architecture of hierarchical triple systems applicable to the HS Hya case. Analyzing the available photometric and spectroscopic data we obtain two main results. First, the dynamical evolution itself allows to constrain the masses of the stars in the inner binary to 1.31 +/- 0.03 M-circle dot and 1.27 +/- 0.03 M-circle dot, and the mass of the unseen third component to 0.56(-0.09)(+0.12)M(circle dot) (all 95% confidence level results). This makes it an M- or K-type dwarf accompanying the binary. Second, the orbital planes of the inner binary and the third component are significantly noncoplanar, allowing two solutions for their mutual angle J. Either the motion of the third component is prograde, and J is most likely in the 50 degrees -65 degrees range, or the motion is retrograde, and J is most likely in the 120 degrees -150 degrees range. The precession period of both orbital planes about the total angular angular momentum is similar to 700 yr (with about two centuries of uncertainty). This implies HS Hya will become eclipsing again around the year 2200.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA21-11058S" target="_blank" >GA21-11058S: Raný orbitální a chemický vývoj planetárních soustav</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

The Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Svazek periodika

163

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

14

Strana od-do

94

Kód UT WoS článku

000750008800001

EID výsledku v databázi Scopus

2-s2.0-85125477118