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Low-mass YSOs with MIDI
László MosoniKonkoly Observatory
Budapest, Hungary
Heidelberg, 2014.05.05
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Projects
MPIA: Ch. Leinert, Th. Ratzka, S. Wolf. Th. HenningLeiden: A. JuhászKonkoly: N. Sipos, K. Gabányi, P. Ábrahám
• radiative transfer modeling of selected objects (V1647 Ori, V883 Ori, AK Sco)
• study of DG Tau• most GTO objects
+ MATISSE (Dutch-connection, MPIA/cryo)
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Dynamics in V1647 Ori
Reipurth & Aspin, 2004 (g',r',i')10”
Hartmann & Kenyon 1996
outburst 2003-2005
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MIDI méréseink
1. 2005 márc. 2. (56m/111deg)
2. 2005 szept. 19. (62m/108deg)
Mosoni, Sipos et al. 20131. faded 2. more extended
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MC3D (Wolf 1999)
RT modeling w MC3D (S. Wolf)• SEDs: 5 epochs• MIDI: 2 epochs
1. reference epoch (SED+MIDI)
„typical” disk & envelope parameters
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MC3D (Wolf 1999)
RT modeling w MC3D (S. Wolf)• SEDs: 5 epochs• MIDI: 2 epochs
1. reference epoch (SED+MIDI)
2. all SEDs
accretion rate changes during the outburst
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MC3D (Wolf 1999)
RT modeling w MC3D (S. Wolf)• SEDs: 5 epochs• MIDI: 2 epochs
1. reference epoch (SED+MIDI)
2. all SEDs
3. 2nd MIDI data
inner radius of dust envelope increased 0.7 AU -> 3.0 AU
• blown-up cavity
• disappearing warm halo
• out-of-equlibrium system
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Other eruptive YSOs with MIDI
• FU Ori (GTO, Quanz et al. 2006)• Z CMa (GTO)• V346 Nor (PI: S. Kraus)• V883 Ori (PI: S. Quanz 2006)
– similar to eruptives (FUor)– observations 2007 Jan. (U2-U3: 44m, U3-U4: 55m)– RT modeling with RADMC (PIs: K. Gabányi & A.
Juhász) – grid – 200 Lsun: stellar or accretion? MIDI cannot distinguish
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V883 Ori
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V883 Ori
left: 0.3M, 300AU
right: 0.4M, 460AU
i=30, 45, 70 deg
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V883 Ori
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V883 Ori
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1. final conclusions from this run, 2. larger grid
V883 Ori
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AK Sco• binary (2 x F5V), a*sini=0.14AU (i~60deg),
= 0.55, d = 145pc (Alencar+ 2003)
• MIDI GTO
• RT modeling(A. Juhász)
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AK Sco
disk – halo degeneracy (+ EX Lupi?)
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AK Sco• binary (2 x F5V), a*sini=0.14AU (i~60deg),
= 0.55, d = 145pc
• MIDI GTO
• RT modeling(K. Gabányi +
A. Juhász)
100pc
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check variations of silicate on UT1-UT2 and UT1-UT3 – finally seven epochs (2012 Oct – 2014 Jan), one with ATs
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Other (GTO) objects
• a few observations per object (10+)• no capacity for RT modeling • survey paper as Boley et al., or Menu et al.?
– what kind of modeling? – include some Hae stars? open time targets?