A theoretical light-curve model for the 1999 outburst of U Scorpii

Izumi Hachisu; Mariko Kato; Taichi Kato; Katsura Matsumoto

A theoretical light-curve model for the 1999 outburst of U Scorpii

Izumi Hachisu, Mariko Kato, Taichi Kato, Katsura Matsumoto

Department of Foreign Languages and Liberal Arts

Research output: Contribution to journal › Article

88 Citations (Scopus)

Abstract

Atheoreticallightcurveforthe1999outburstofUScorpiiispresentedinordertoobtai nvariousphysicalparametersoftherecurrentnova. OurUScomodelconsistsofaverymassivewhitedwarf(WD)withanaccretiondiskandalobe- filling,slightlyevolved,main-sequencestar(MS). Themodelincludesareflectioneffectbythecompanionandtheaccretiondisktogetherwithas hadowingeffectonthecompanionbytheaccretiondisk. Theearlyvisuallightcurve(withalinearphaseoft∼1-15daysaftermaximum) iswellreproducedbyathermonuclearrunawaymodelonaverymassiveWDclosetotheChandrasek harlimit(M _WD=1.37±0.01M⊙), inwhichopticallythickwindsblowingfromtheWDplayakeyroleindeterminingthenovadurati on.Theensuingplateauphase(t∼15-30days) isalsoreproducedbythecombinationofaslightlyirradiatedMSandafullyirradiatedflarin g-updiskwitharadius∼1.4timestheRochelobesize.Thecoolingphase(t∼30- 40days)isconsistentwithalow-hydrogencontentofX≈0.05oftheenvelopeforthe1. 37M⊙WD.Thebest-fitparametersaretheWDmassofM _WD∼1.37M⊙,thecompanionmassofM _MS∼1.5M⊙(0.8-2.0M⊙isacceptable), theinclinationangleoftheorbit(i∼80°),andtheflaring-upedge, theverticalheightofwhichis∼0.30timestheaccretiondiskradius. Thedurationofthestrongwindphase(t∼0-17days) isveryconsistentwiththeBeppoSAXsupersoftX-raydetectionatt∼19- 20daysbecausesupersoftX-raysareself-absorbedbythemassivewind. Theenvelopemassatthepeakisestimatedtobe∼3×10 ^-6M⊙,whichisindicatesanaveragemassaccretionrateof∼2. 5×10^-7M⊙yr ^-1duringthequiescentphasebetween1987and1999. ThesequantitiesareexactlythesameasthosepredictedinanewprogenitormodelofTypeIasup ernovae.

Original language	English
Pages (from-to)	L97-L100
Journal	Astrophysical Journal
Volume	528
Issue number	2 PART 2
Publication status	Published - 2000 Jan 10

Keywords

Accretion, accretion disks
Binaries: close
Novae, cataclysmic variables
Stars: individual (U Scorpii)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

Fingerprint Dive into the research topics of 'A theoretical light-curve model for the 1999 outburst of U Scorpii'. Together they form a unique fingerprint.

Cite this

Hachisu, I., Kato, M., Kato, T., & Matsumoto, K. (2000). A theoretical light-curve model for the 1999 outburst of U Scorpii. Astrophysical Journal, 528(2 PART 2), L97-L100.

@article{3f3e69d50a6f4875a586b7a5a00be08e,

title = "A theoretical light-curve model for the 1999 outburst of U Scorpii",

abstract = "Atheoreticallightcurveforthe1999outburstofUScorpiiispresentedinordertoobtai nvariousphysicalparametersoftherecurrentnova. OurUScomodelconsistsofaverymassivewhitedwarf(WD)withanaccretiondiskandalobe- filling,slightlyevolved,main-sequencestar(MS). Themodelincludesareflectioneffectbythecompanionandtheaccretiondisktogetherwithas hadowingeffectonthecompanionbytheaccretiondisk. Theearlyvisuallightcurve(withalinearphaseoft∼1-15daysaftermaximum) iswellreproducedbyathermonuclearrunawaymodelonaverymassiveWDclosetotheChandrasek harlimit(M WD=1.37±0.01M⊙), inwhichopticallythickwindsblowingfromtheWDplayakeyroleindeterminingthenovadurati on.Theensuingplateauphase(t∼15-30days) isalsoreproducedbythecombinationofaslightlyirradiatedMSandafullyirradiatedflarin g-updiskwitharadius∼1.4timestheRochelobesize.Thecoolingphase(t∼30- 40days)isconsistentwithalow-hydrogencontentofX≈0.05oftheenvelopeforthe1. 37M⊙WD.Thebest-fitparametersaretheWDmassofM WD∼1.37M⊙,thecompanionmassofM MS∼1.5M⊙(0.8-2.0M⊙isacceptable), theinclinationangleoftheorbit(i∼80°),andtheflaring-upedge, theverticalheightofwhichis∼0.30timestheaccretiondiskradius. Thedurationofthestrongwindphase(t∼0-17days) isveryconsistentwiththeBeppoSAXsupersoftX-raydetectionatt∼19- 20daysbecausesupersoftX-raysareself-absorbedbythemassivewind. Theenvelopemassatthepeakisestimatedtobe∼3×10 -6M⊙,whichisindicatesanaveragemassaccretionrateof∼2. 5×10-7M⊙yr -1duringthequiescentphasebetween1987and1999. ThesequantitiesareexactlythesameasthosepredictedinanewprogenitormodelofTypeIasup ernovae.",

keywords = "Accretion, accretion disks, Binaries: close, Novae, cataclysmic variables, Stars: individual (U Scorpii)",

author = "Izumi Hachisu and Mariko Kato and Taichi Kato and Katsura Matsumoto",

year = "2000",

month = jan,

day = "10",

language = "English",

volume = "528",

pages = "L97--L100",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "2 PART 2",

}

TY - JOUR

T1 - A theoretical light-curve model for the 1999 outburst of U Scorpii

AU - Hachisu, Izumi

AU - Kato, Mariko

AU - Kato, Taichi

AU - Matsumoto, Katsura

PY - 2000/1/10

Y1 - 2000/1/10

N2 - Atheoreticallightcurveforthe1999outburstofUScorpiiispresentedinordertoobtai nvariousphysicalparametersoftherecurrentnova. OurUScomodelconsistsofaverymassivewhitedwarf(WD)withanaccretiondiskandalobe- filling,slightlyevolved,main-sequencestar(MS). Themodelincludesareflectioneffectbythecompanionandtheaccretiondisktogetherwithas hadowingeffectonthecompanionbytheaccretiondisk. Theearlyvisuallightcurve(withalinearphaseoft∼1-15daysaftermaximum) iswellreproducedbyathermonuclearrunawaymodelonaverymassiveWDclosetotheChandrasek harlimit(M WD=1.37±0.01M⊙), inwhichopticallythickwindsblowingfromtheWDplayakeyroleindeterminingthenovadurati on.Theensuingplateauphase(t∼15-30days) isalsoreproducedbythecombinationofaslightlyirradiatedMSandafullyirradiatedflarin g-updiskwitharadius∼1.4timestheRochelobesize.Thecoolingphase(t∼30- 40days)isconsistentwithalow-hydrogencontentofX≈0.05oftheenvelopeforthe1. 37M⊙WD.Thebest-fitparametersaretheWDmassofM WD∼1.37M⊙,thecompanionmassofM MS∼1.5M⊙(0.8-2.0M⊙isacceptable), theinclinationangleoftheorbit(i∼80°),andtheflaring-upedge, theverticalheightofwhichis∼0.30timestheaccretiondiskradius. Thedurationofthestrongwindphase(t∼0-17days) isveryconsistentwiththeBeppoSAXsupersoftX-raydetectionatt∼19- 20daysbecausesupersoftX-raysareself-absorbedbythemassivewind. Theenvelopemassatthepeakisestimatedtobe∼3×10 -6M⊙,whichisindicatesanaveragemassaccretionrateof∼2. 5×10-7M⊙yr -1duringthequiescentphasebetween1987and1999. ThesequantitiesareexactlythesameasthosepredictedinanewprogenitormodelofTypeIasup ernovae.

AB - Atheoreticallightcurveforthe1999outburstofUScorpiiispresentedinordertoobtai nvariousphysicalparametersoftherecurrentnova. OurUScomodelconsistsofaverymassivewhitedwarf(WD)withanaccretiondiskandalobe- filling,slightlyevolved,main-sequencestar(MS). Themodelincludesareflectioneffectbythecompanionandtheaccretiondisktogetherwithas hadowingeffectonthecompanionbytheaccretiondisk. Theearlyvisuallightcurve(withalinearphaseoft∼1-15daysaftermaximum) iswellreproducedbyathermonuclearrunawaymodelonaverymassiveWDclosetotheChandrasek harlimit(M WD=1.37±0.01M⊙), inwhichopticallythickwindsblowingfromtheWDplayakeyroleindeterminingthenovadurati on.Theensuingplateauphase(t∼15-30days) isalsoreproducedbythecombinationofaslightlyirradiatedMSandafullyirradiatedflarin g-updiskwitharadius∼1.4timestheRochelobesize.Thecoolingphase(t∼30- 40days)isconsistentwithalow-hydrogencontentofX≈0.05oftheenvelopeforthe1. 37M⊙WD.Thebest-fitparametersaretheWDmassofM WD∼1.37M⊙,thecompanionmassofM MS∼1.5M⊙(0.8-2.0M⊙isacceptable), theinclinationangleoftheorbit(i∼80°),andtheflaring-upedge, theverticalheightofwhichis∼0.30timestheaccretiondiskradius. Thedurationofthestrongwindphase(t∼0-17days) isveryconsistentwiththeBeppoSAXsupersoftX-raydetectionatt∼19- 20daysbecausesupersoftX-raysareself-absorbedbythemassivewind. Theenvelopemassatthepeakisestimatedtobe∼3×10 -6M⊙,whichisindicatesanaveragemassaccretionrateof∼2. 5×10-7M⊙yr -1duringthequiescentphasebetween1987and1999. ThesequantitiesareexactlythesameasthosepredictedinanewprogenitormodelofTypeIasup ernovae.

KW - Accretion, accretion disks

KW - Binaries: close

KW - Novae, cataclysmic variables

KW - Stars: individual (U Scorpii)

UR - http://www.scopus.com/inward/record.url?scp=0034627510&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0034627510&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0034627510

VL - 528

SP - L97-L100

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART 2

ER -