light curves of the dwarf nova u gem: a diagnostic of accretion disk evolution
DESCRIPTION
Light Curves of the Dwarf Nova U Gem: A Diagnostic of Accretion Disk Evolution. Larry Molnar Calvin College Grand Rapids, Michigan. Outline. Calvin-Rehoboth Twin Telescopes Project Dwarf Novae U Gem Preliminary Light Curves. Calvin-Rehoboth Twin Telescope Project. NSF-CCLI funding - PowerPoint PPT PresentationTRANSCRIPT
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Light Curves of the Dwarf Nova U Gem: A Diagnostic of Accretion Disk Evolution
Larry MolnarCalvin CollegeGrand Rapids,Michigan
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Outline
• Calvin-Rehoboth Twin Telescopes Project• Dwarf Novae• U Gem• Preliminary Light Curves
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Calvin-Rehoboth Twin Telescope Project
• NSF-CCLI funding• Two 16” OGS telescopes
– One in Grand Rapids, MI• Hands-on experience for students• Development platform for remote site
– One in Rehoboth, NM (35.5N,108.6W)• Unattended robotic operation• High throughput
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Dwarf Novae
• White dwarf + red dwarf• Red dwarf fills Roche Lobe• Angular momentum loss leads to mass
transfer via an accretion stream, and formation of an accretion disk
• Disk conditions do not permit steady-state
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U Gem
• Brightness: 10-14 magnitude• Mass ratio: 0.25• Orbital period: 4.24 hours• Outburst time scale: 3-4 months• Inclination: hot spot is eclipsed by red
dwarf
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10
10.5
11
11.5
12
12.5
13
13.5
14
2453020 2453030 2453040 2453050 2453060 2453070 2453080 2453090
Julian DateI (
mag
)
U Gem
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12.6
12.7
12.8
12.9
13.0
13.1
13.2
13.3
13.4
13.5
2453078.55 2453078.60 2453078.65 2453078.70 2453078.75 2453078.80 2453078.85
Julian Date [3/13/4]
I (m
ag)
U Gem
Check 6
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10.1
10.3
10.5
10.7
10.9
11.1
11.3
-0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8
Orbital Phase
I (m
ag)
3/7/43/8/43/9/4
U Gem
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12.8
13
13.2
13.4
13.6
-0.8 -0.6 -0.4 -0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2
Orbital Phase
I (m
ag)
1/18/43/13/43/15/43/20/4
U Gem
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12.9
13
13.1
13.2
13.3
13.4
-0.20 -0.15 -0.10 -0.05 0.00 0.05 0.10 0.15 0.20
Orbital Phase
I (m
ag)
1/18/43/13/43/15/43/20/4
U Gem
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Conclusions
• U Gem data demonstrate capabilities of new system
• Comparison of eclipses before and after outburst are consistent with accretion disk radius increasing gradually through the quiescent phase