WZ Sge-Type Star V592 Herculis
We observed the entire course of the 1998 outburst of V592 Her, which was originally reported as a nova in 1968. We have been able to construct a full light curve of the outburst, which is characterized by a rapid initial decline (0.98 mag/d), which smoothly developed into a plateau phase with a slo...
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| creator | Kato, T Uemura, M Matsumoto, K Kinnunen, T Garradd, G Masi, G Yamaoka, H |
| description | We observed the entire course of the 1998 outburst of V592 Her, which was
originally reported as a nova in 1968. We have been able to construct a full
light curve of the outburst, which is characterized by a rapid initial decline
(0.98 mag/d), which smoothly developed into a plateau phase with a slower
linear decline. We detected superhumps characteristic to SU UMa-type dwarf
novae ~7 d after the optical maximum. The overall behavior of the light curve
and the development of superhumps were characteristic to a WZ Sge-type dwarf
nova. Combined with the past literature, we have been able to uniquely
determine the superhump period to be 0.05648(2) d. From this period, together
with a modern interpretation of the absolute magnitude of the outburst light
curve, we conclude that the overall picture of V592 Her is not inconsistent
with a lower main-sequence secondary star in contrast to a previous claim that
V592 Her contains a brown dwarf. |
| doi_str_mv | 10.48550/arxiv.astro-ph/0209283 |
| format | Article |
| fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_astro_ph_0209283</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>astro_ph_0209283</sourcerecordid><originalsourceid>FETCH-arxiv_primary_astro_ph_02092833</originalsourceid><addsrcrecordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNA3MDKwNLIw5mSQC49SCE5P1Q2pLEhVCC5JLFIIM7U0UvBILUouzcks5mFgTUvMKU7lhdLcDKpuriHOHrpg8-ILijJzE4sq48HmxhdkxEPNNSZWHQAGKjFp</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>WZ Sge-Type Star V592 Herculis</title><source>arXiv.org</source><creator>Kato, T ; Uemura, M ; Matsumoto, K ; Kinnunen, T ; Garradd, G ; Masi, G ; Yamaoka, H</creator><creatorcontrib>Kato, T ; Uemura, M ; Matsumoto, K ; Kinnunen, T ; Garradd, G ; Masi, G ; Yamaoka, H</creatorcontrib><description>We observed the entire course of the 1998 outburst of V592 Her, which was
originally reported as a nova in 1968. We have been able to construct a full
light curve of the outburst, which is characterized by a rapid initial decline
(0.98 mag/d), which smoothly developed into a plateau phase with a slower
linear decline. We detected superhumps characteristic to SU UMa-type dwarf
novae ~7 d after the optical maximum. The overall behavior of the light curve
and the development of superhumps were characteristic to a WZ Sge-type dwarf
nova. Combined with the past literature, we have been able to uniquely
determine the superhump period to be 0.05648(2) d. From this period, together
with a modern interpretation of the absolute magnitude of the outburst light
curve, we conclude that the overall picture of V592 Her is not inconsistent
with a lower main-sequence secondary star in contrast to a previous claim that
V592 Her contains a brown dwarf.</description><identifier>DOI: 10.48550/arxiv.astro-ph/0209283</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics</subject><creationdate>2002-09</creationdate><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,881</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/astro-ph/0209283$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.1093/pasj/54.6.999$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.astro-ph/0209283$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Kato, T</creatorcontrib><creatorcontrib>Uemura, M</creatorcontrib><creatorcontrib>Matsumoto, K</creatorcontrib><creatorcontrib>Kinnunen, T</creatorcontrib><creatorcontrib>Garradd, G</creatorcontrib><creatorcontrib>Masi, G</creatorcontrib><creatorcontrib>Yamaoka, H</creatorcontrib><title>WZ Sge-Type Star V592 Herculis</title><description>We observed the entire course of the 1998 outburst of V592 Her, which was
originally reported as a nova in 1968. We have been able to construct a full
light curve of the outburst, which is characterized by a rapid initial decline
(0.98 mag/d), which smoothly developed into a plateau phase with a slower
linear decline. We detected superhumps characteristic to SU UMa-type dwarf
novae ~7 d after the optical maximum. The overall behavior of the light curve
and the development of superhumps were characteristic to a WZ Sge-type dwarf
nova. Combined with the past literature, we have been able to uniquely
determine the superhump period to be 0.05648(2) d. From this period, together
with a modern interpretation of the absolute magnitude of the outburst light
curve, we conclude that the overall picture of V592 Her is not inconsistent
with a lower main-sequence secondary star in contrast to a previous claim that
V592 Her contains a brown dwarf.</description><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2002</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNA3MDKwNLIw5mSQC49SCE5P1Q2pLEhVCC5JLFIIM7U0UvBILUouzcks5mFgTUvMKU7lhdLcDKpuriHOHrpg8-ILijJzE4sq48HmxhdkxEPNNSZWHQAGKjFp</recordid><startdate>20020915</startdate><enddate>20020915</enddate><creator>Kato, T</creator><creator>Uemura, M</creator><creator>Matsumoto, K</creator><creator>Kinnunen, T</creator><creator>Garradd, G</creator><creator>Masi, G</creator><creator>Yamaoka, H</creator><scope>GOX</scope></search><sort><creationdate>20020915</creationdate><title>WZ Sge-Type Star V592 Herculis</title><author>Kato, T ; Uemura, M ; Matsumoto, K ; Kinnunen, T ; Garradd, G ; Masi, G ; Yamaoka, H</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_astro_ph_02092833</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2002</creationdate><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Kato, T</creatorcontrib><creatorcontrib>Uemura, M</creatorcontrib><creatorcontrib>Matsumoto, K</creatorcontrib><creatorcontrib>Kinnunen, T</creatorcontrib><creatorcontrib>Garradd, G</creatorcontrib><creatorcontrib>Masi, G</creatorcontrib><creatorcontrib>Yamaoka, H</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Kato, T</au><au>Uemura, M</au><au>Matsumoto, K</au><au>Kinnunen, T</au><au>Garradd, G</au><au>Masi, G</au><au>Yamaoka, H</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>WZ Sge-Type Star V592 Herculis</atitle><date>2002-09-15</date><risdate>2002</risdate><abstract>We observed the entire course of the 1998 outburst of V592 Her, which was
originally reported as a nova in 1968. We have been able to construct a full
light curve of the outburst, which is characterized by a rapid initial decline
(0.98 mag/d), which smoothly developed into a plateau phase with a slower
linear decline. We detected superhumps characteristic to SU UMa-type dwarf
novae ~7 d after the optical maximum. The overall behavior of the light curve
and the development of superhumps were characteristic to a WZ Sge-type dwarf
nova. Combined with the past literature, we have been able to uniquely
determine the superhump period to be 0.05648(2) d. From this period, together
with a modern interpretation of the absolute magnitude of the outburst light
curve, we conclude that the overall picture of V592 Her is not inconsistent
with a lower main-sequence secondary star in contrast to a previous claim that
V592 Her contains a brown dwarf.</abstract><doi>10.48550/arxiv.astro-ph/0209283</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
| title | WZ Sge-Type Star V592 Herculis |
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