Dense spot coverage and polar caps on SV Cam

S V  Jeffers; A C  Cameron; J R  Barnes; J P  Aufdenberg; G A J  Hussain

Dense spot coverage and polar caps on SV Cam

S V Jeffers, A C Cameron, J R Barnes, J P Aufdenberg, G A J Hussain

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

We have used spectrophotometric data from 9 HST orbits to eclipse-map the primary component of the RS CVn binary SV Cam. From these observations and SV Cam's HIPPARCOS parallax we find that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. The flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. Even when we extend the spottedness from the eclipsed region to the entire surface, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48 +/- 6 degrees.

Original language	English
Title of host publication	Procs of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
Editors	F Favata, G A J Hussain, B Battrick
Place of Publication	PARIS
Publisher	European Space Agency (ESA)
Pages	669-671
Number of pages	3
ISBN (Print)	92-9092-871-9
Publication status	Published - 2005
Event	13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - Hamburg Duration: 5 Jul 2004 → 9 Jul 2004

Conference

Conference	13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
City	Hamburg
Period	5/07/04 → 9/07/04

Keywords

stars : activity
stars : spots binaries : eclipsing
STARS

Cite this

@inproceedings{1b4d134585f5418cab89b0166b44891c,

title = "Dense spot coverage and polar caps on SV Cam",

abstract = "We have used spectrophotometric data from 9 HST orbits to eclipse-map the primary component of the RS CVn binary SV Cam. From these observations and SV Cam's HIPPARCOS parallax we find that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. The flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. Even when we extend the spottedness from the eclipsed region to the entire surface, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48 +/- 6 degrees.",

keywords = "stars : activity, stars : spots binaries : eclipsing, STARS",

author = "Jeffers, {S V} and Cameron, {A C} and Barnes, {J R} and Aufdenberg, {J P} and Hussain, {G A J}",

year = "2005",

language = "English",

isbn = "92-9092-871-9",

pages = "669--671",

editor = "F Favata and Hussain, {G A J} and B Battrick",

booktitle = "Procs of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun",

publisher = "European Space Agency (ESA)",

address = "Netherlands",

note = "13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun ; Conference date: 05-07-2004 Through 09-07-2004",

}

Jeffers, SV, Cameron, AC, Barnes, JR, Aufdenberg, JP & Hussain, GAJ 2005, Dense spot coverage and polar caps on SV Cam. in F Favata, GAJ Hussain & B Battrick (eds), Procs of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. European Space Agency (ESA), PARIS, pp. 669-671, 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, Hamburg, 5/07/04.

TY - GEN

T1 - Dense spot coverage and polar caps on SV Cam

AU - Jeffers, S V

AU - Cameron, A C

AU - Barnes, J R

AU - Aufdenberg, J P

AU - Hussain, G A J

PY - 2005

Y1 - 2005

N2 - We have used spectrophotometric data from 9 HST orbits to eclipse-map the primary component of the RS CVn binary SV Cam. From these observations and SV Cam's HIPPARCOS parallax we find that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. The flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. Even when we extend the spottedness from the eclipsed region to the entire surface, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48 +/- 6 degrees.

AB - We have used spectrophotometric data from 9 HST orbits to eclipse-map the primary component of the RS CVn binary SV Cam. From these observations and SV Cam's HIPPARCOS parallax we find that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. The flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. Even when we extend the spottedness from the eclipsed region to the entire surface, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48 +/- 6 degrees.

KW - stars : activity

KW - stars : spots binaries : eclipsing

KW - STARS

M3 - Conference contribution

SN - 92-9092-871-9

SP - 669

EP - 671

BT - Procs of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun

A2 - Favata, F

A2 - Hussain, G A J

A2 - Battrick, B

PB - European Space Agency (ESA)

CY - PARIS

T2 - 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun

Y2 - 5 July 2004 through 9 July 2004

ER -

Dense spot coverage and polar caps on SV Cam

Abstract

Conference

Keywords

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