A New Mechanism o Fo ming Ho Co inos:
Shocks om Bina y In e ac ions
Munan Gong
Max Planck Ins i u e o Ex a e es ial Physics (MPE)
Wi h Ma ia Jose Mau ei a, Paola Caselli, Joaquin Zamponi (MPE), Lo enz Gae ne (LMU),
Kai lin K a e (A izona), Ked on Silsbee (UTEP)
Towa ds New F on ie s, ESO, 11 Ma ch, 2025
The deeply embedded P o os ella Disk IRAS 16293-2422
Slide c edi : Ma ia Jose Mau ei a (MPE)
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
Slide c edi : Ma ia Jose Mau ei a (MPE)
The deeply embedded P o os ella Disk IRAS 16293-2422
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
Cazaux e al. (2003)
…we conclude ha he high abundance o complex
species in he ho co e a ound IRAS 16293 implies he
e apo a ion o ice in o he wa m gas.
— Cazaux e al. (2003)
The Fi s De ec ion o Complex O ganic Molecule (COM) Emissions owa ds a Low Mass P o os a
Caselli & Cecca elli (2012)
I e iew wha we know oday abou he inne wa m egions o sola ype p o os a s.
I will call hese egions “ho co inos" o dis inguish hem om massi e ho co es.
— Cecca elli e al. (2004)
I e iew wha we know oday abou he inne wa m egions o sola ype p o os a s.
I will call hese egions “ho co inos" o dis inguish hem om massi e ho co es.
— Cecca elli e al. (2004)
High Mass P o os a + COM Emission = “Ho Co e”
Low Mass P o os a + COM Emission = “Ho Co ino”
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
Cazaux e al. (2003)
…we conclude ha he high abundance o complex
species in he ho co e a ound IRAS 16293 implies he
e apo a ion o ice in o he wa m gas.
— Cazaux e al. (2003)
The Name o “Ho Co ino”
Caselli & Cecca elli (2012)
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
Physical Model o IRAS 16293
Do y e al. (2004),
See also Schöie e al. (2002), Cecca elli e a. (2000)
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
Mul iple Ho Co inos
ALMA con inuum
Jo gensen e al. 2016, Mau ei a, Gong e al. 2020a
141 au
Fo es o COM lines
Manigand e al. 2020
Spa ial dis ibu ion o
COMs poo ly esol ed
Oya e al. 2018
4-6 Msun wi hin
ew 1,000 au
0.14 pc
He schel column densi y!
Ladjela e e al. 2020
ALMA con inuum
Jo gensen e al. 2016, Mau ei a, Gong e al. 2020a
141 au
A T iple Sys em: Bina y + Companion
ALMA con inuum
Jo gensen e al. 2016, Mau ei a e al. 2020, 2022
141 au
Ho Spo s in he Ci cumbina y Disk o IRAS 16293 A
Mau ei a e al. (2018)
Mau ei a, Gong e al. (2022)
•Wha is he o igin o he ho spo s?
Hin s o Bina y Shocks in Class 0/I P o os ella Disks
Al es e al. (2019), Vas el e al. (2025)
BHB2007, CH3OH emission nea one spi al ea u e
Hsieh e al. (2025)
SVS13A, CH3CN emission in he
“b idge” be ween wo p o os a s
Take Home Messages: The Keys o Modelling P o os ella Disks
I. Dynamics Rules
Radia i e Hea ing,
Dus , Chemis y…
+
Young Disks a e No Passi e
Dynamical E ec s:
- Shocks (Mau ei a e al. 2022, Gong e al.
in p ep)
- Acc e ion Hea ing (Zamponi e al. 2021,
Lin e al. 2020)
Disks a e NOT iso he mal/locally iso he mal
II. Simula ion Needs The modynamics
T ≠ cons an
I is Impo an o include hea ing and
cooling in hyd odynamical simula ions
We need bo h high- esolu ion
obse a ions and ealis ic simula ions
III. Obse a ion + Simula ion
Q1: Wha causes ho spo s in bina y p o os ella disks?
•A. Aliens ying o ge WIFI om hei phones
•B. Shocks c ea ed by he g a i a ional in e ac ion be ween he gas and he bina y s a s
Q2: How can we unde s and p o os ella disks?
•A. By conduc ing high esolu ion obse a ions o dus and molecula lines
•B. By building ealis ic nume ical simula ions wi h he modynamics
•C. By combining obse a ions and simula ions
•D. All o he abo e
Summa y
Quiz!
