Manuel Pichardo Marcano (he/him)

Manuel Pichardo Marcano

Text

Estudio Binarias Compactas

Caltech

NASA

Credits: NASA/Rivera Sandoval

Cúmulos Globulares

47 Tuc en Rayos X

47 Tuc en Óptico

Estudio Binarias Compactas

2- SCOVaS: Survey for Compact Objects and Variables

Pichardo Marcano et al. (2021a)

Pichardo Marcano et al. (2023)

   Pichardo Marcano et al. (in prep.)

1- TACOS: TESS AM CVn Outbursts Survey

Pichardo Marcano et al. (2021b)

Caltech

NASA

¿Qué es una Estrella?

• Objeto celeste autogravitatorio:
  • unido por la atracción gravitacional de sus partes.
• Hay, o hubo una vez fusión termonuclear sostenida de hidrógeno en su núcleo.

Estrellas

El Sol

Enana Blanca Y

Estrella de Neutrones

No Estrellas

No Todas son Iguales

Diferencias:

• Brillo Aparente:
  • Brillo ∝ 1/distancia²
  • Distancia:
    • Luminosidad (Brillo intrínseco) [Vatios]
    • L ∝ R² T⁴
  • Color
    • Temperatura
  • Masa y Radio
    • Difíciles de Medir

25 Estrellas Más Brillantes

El Sol como una estrella

Nuestro Referente Estelar

Luminosidad Solar = 1 L☉ = 3.8 x 10²⁶ Vatios

Masa Solar = 1 M☉ = 1.988 x 10³⁰ Kg

Radio Solar = 1 R☉ = 695700 km

Temperatura ∼ 5772 K = 5498.85 C

Medir la temperatura del Sol

Todo lo que tiene temperatura > 0 K emite radiación (luz)

Medir la temperatura del Sol

Todo lo que tiene temperatura > 0 K emite radiación (luz)

Radiación de cuerpo negro

Medir la temperatura del Sol

El Color Depende de la Temperatura

Radiación de cuerpo negro

Necesitamos la Distancia

¿Cómo medir la Luminosidad?

Brillo ∝ L/distancia ²

Luminosidad ∝ Brillo X distancia ²

1 L☉

Gaia

El Cartógrafo de la Vía Láctea

•  Telescopio espacial de la Agencia Espacial Europea (ESA)
• ∼ 2 mil millones de estrellas
  • Distancias, Colores, Brillos Aparentes, Movimientos Propios

El paralaje

Gaia

¿Cómo Gaia mide distancias?

Gaia

¿Cómo Gaia mide distancias?

El paralaje

Gaia

¿Cómo Gaia mide Colores (temperatura)?

Filtros

• Gaia tiene 3 Filtros:
  • G, BP (Azul), RP (Rojo)

Longitud de Onda

El Diagrama H-R de Gaia

Azul <-

Rojo ->

Más Luminosas

Menos Luminosas

 <- Más Calientes

El Diagrama H-R de Gaia

Azul <-

Rojo ->

Más Luminosas

Menos Luminosas

 <- Más Calientes

Gigantes

La Secuencia Principal

Estrellas Masivas

.

Estrellas de Baja Masa

1 M☉

50 M☉

0.5 M☉

La Secuencia Principal

Estrellas "Normales"

• Sostenidas por Fusión Nuclear:
  • H-> He
• Pasan la mayor parte de su vida
  • L ∝ M⁴
  • Estrellas Masivas Viven Menos

La Secuencia Principal

Azul <-

Rojo ->

¿Qué son estas letras?

Clasificación de Las Estrellas

Las Estrellas se clasifican de acuerdo a sus Espectros

Se pasa la luz por un "prisma"

El Espectro del Sol

La Huella Digital de las Estrellas

Las "Computadoras" de Harvard

Annie Jump Cannon:

Desarrolló el sistema de clasificación basado en Temperatura

O B A F G K M

Clasificación de las estrellas

   Temperatura                            

Clasificación de las estrellas

Clasificación de las estrellas

¿Por que los espectros se ven diferentes?

Cecilia Payne-Gaposchkin:

• La mujer que descubrió la composición de las estrellas.
• Primera interpretación teórica de los espectros.

El Ciclo de Vida del Sol

¿Qué pasa cuando se le acaba el Hidrógeno?

El Sol y la mayoría de las estrellas del universo terminaran como una enana blanca

El Ciclo de Vida del Sol

El Ciclo de Vida del Sol

Nucleo Inerte

de He

Capa Fusionando H->He

Capa Exterior

Extendida

El Ciclo de Vida del Sol

Tope Rama Gigante Roja

Base Rama Gigante Roja

Subgigante

El Ciclo de Vida del Sol

El Ciclo de Vida del Sol

Rama Gigante Roja

Flash de Helio

Rama Horizontal​

El Ciclo de Vida del Sol

Núcleo Fusionando

He

Capa Fusionando H->He

Capa Exterior

Extendida

• Helio se convierte en Carbono

El Ciclo de Vida del Sol

Nucleo Inerte

de C

Capa Fusionando H->He

Capa Fusionando He

Capa Exterior

Extendida

El Ciclo de Vida del Sol

Rama Asintótica Gigante

El Ciclo de Vida del Sol

Origen de los elementos

El Ciclo de Vida del Sol

Nebulosa Planetaria

El Ciclo de Vida del Sol

Enana Blanca

Enanas Blancas

Masa ~ 1 M☉

Radio ~ 1 R🜨

Radio ~ 1 R🜨

Estrellas "Muertas"

Masa ~ 1 M☉

Radio ~ 1 R🜨

Radio ~ 1 R🜨

Presión Electrones

Fusión Nuclear

El Ciclo de Vida del Sol

Nebulosa Planetaria

RH

El Ciclo de Vida de Millones

RGB = Rama de Gigante Roja

HB = Rama Horizontal

AGB = Rama Asintótica Gigante

Azul <-

Rojo ->

Resumen

Cosas de las que no hablé

• Evolución Estrellas Masivas:
  • Supernovas
  • Hoyos Negros
  • Estrellas de Neutrones
• Evolución Estrellas Mediana Masa:
  • Enanas Blancas Masivas
  • Supergigante Rojas
• Evolución Binaria
  • Formación de binarias compactas
  • Fuentes de ondas gravitacionales

Cosas de las que sí hablé

• Gaia
  • Cartógrafo de la Vía Lactea
• El Diagrama H-R:
  • Diagrama más importante/útil para la astronomía estelar
• Clasificación de Estrellas:
  • Espectros
• Ciclo de Vida del Sol:
  • Estrellas de baja masa
  • Estrellas más comunes

Manuel Pichardo Marcano

Email: manuelpichardom@gmail.com

Extra

Accreting White Dwarf Binaries

Cataclysmic Variables

AM CVn

• Main Sequence Star
• P_orb ~ 80 min - 10 hours
• Outbursts:
  • 2-20 days
  • Disk instability model+ (DIM)
• >1000 in the galactic field
• Predicted large # in old Star Clusters

• White Dwarf/Helium Star
• P_orb ~ 5 - 70 min
• Outburts:
  • weeks?
  • DIM?
• ~70 in the galactic field

Mark A. Garlick

Caltech

AM Canum Venaticorum AM CVn

• White dwarf + White dwarf

• White dwarf + He Star

• Orbital Period: 5-70 minutes

• Rare: 70 Galactic field

Transiting Exoplanet Survey Satellite TESS

TESS Cadence and Coverage

• Primary mission:
  • 2-min selected targets
  • 30-min full-frame images (FFI).
• Extended:
  • 20 sec selected targets
  • 10-min FFI
• Second extended mission
  • 200-second FFI

Disk AM CVns

High state (high Ṁ)

• Hot ionized disk

~20

~10

~40-60 (?)

Low state (low Ṁ)

• Cold stable disk

Caltech

Outbursts

Pichardo Marcano et al. (2021)

SO duration

• Precursor
  • TESS (Duffy et al. 2021)
• 5/6 have Precursor
  • Except ASASSN-14cc

PTF1 J0719+4858

Pichardo Marcano et al. (2021)

ZTF

TESS

Precursor

Type of Super Outbursts

Osaki et al. (2005)

High Mass Ratio

DIM

Cataclysmic Variables

See also Duffy et al. (2021)

High Mass Ratio

High Mass Ratio

High Mass Ratio

 eccentric disc develops rapidly

Type of Echo Outbursts

SDSS J1043+5632

• P_orb = 28.5 min
• WZ Sge like
  • Precursors
  • EMT (Hameury+'20)
  • Reflection:
    • Hot Massive WD

• P_orb = 26.7 min
• Compare to TCP J21040470+4631129
  • EMT (Hameury+'20)
• Helium "SU UMa"
  • EMT+TTI (Kotko+'12)

SO

rebrightening

SO

rebrightening

• Color Evolution

PTF1 J0719+4858

Pichardo Marcano et al. (2021)

ZTF

SO

NO

SO

NO

rebrightening

rebrightening

Color Evolution

PTF1 J0719+4858

• Similar to Dwarf Novae

  • Hameury et al. (2020)

• Similar SDSS J1411+4812
  • Rivera Sandoval et al. (2021)
• Compare to SDSS 1137
  • Rivera Sandoval et al. (2021)

Pichardo Marcano et al. (2021)

SDSS J113732+405458

 Enhanced mass transfer

Rivera Sandoval et al. (2021)

P_orb = 26.7 min

P_orb ~ 60 min

Superoutburst duration vs P_orb

Pichardo Marcano et al. (2021)

Cataclysmic Variables

• White dwarf primary

• "Main-sequence" donor

• Roche-lobe overflow

• Accretion disk (non-magnetic)

• Highly Variables:

  • Dwarf novae

    • 2-8 mag outburst

    • 10-100 increase in L

Looking of CVs in GCs

NASA, ESA, H. Richer and J. Heyl (University of British Columbia), and J. Anderson and J. Kalirai (STScI)

Finding CVs in X-rays and UV

• Advantages of X-ray Searches:

  • Avoid crowding

• Disadvantages:

  • Small FoV (FUV)
  • Lx ≥ 10²⁹ ergs/s

Summary CVs in GCs

• Few of CVs per cluster

• X-ray biased sample:

  • Lx > 10²⁹ergs/s

• Dearth of DNe:

  • Only 17 confirmed

• Core-collapsed:

  • Bimodal population

• Non core-collapsed:

  • 1 faint population

• Period distribution?

  • 16 known periods

All Magnetics ?

• HST Archive
• 7 Globular Clusters
• Many Exposures
• Different properties
  • Metallicity
  • Core-collapsed
  • Non core-collapsed

SCOVaS: Survey for Compact Objects and Variables

Preliminary Results

NGC 6397

• Closest Core Collapse
• Second Closest
  • 2.4 kpc
  • 15 CV candidates
  • 2 Pulsars

Preliminary Results

NGC 6397

We haven't found new

X-ray faint CVs

Spoiler Alert!

Other Binaries

Credits: NASA/Rivera Sandoval

Main et al 2018 (Nature)

Redback 'spider' Pulsar

Redback  Pulsar

A new candidate Redback MSP

Pichardo Marcano et. al (2021a)

• Porb 1.96 days
• Longest Porb for Redback in GCs
• Missed MSP in Pulsar Searchers
  • Confirmed by Zhang et al. (2022)

Magnetic He WD Candidate

• V_rad > 150 km/s (MUSE)
• Not Detected in X-rays
  • Lx < 10²⁸ ergs/s
• Roche-lobe filling stripped star?
  • M~ 2 x 10^-4 ☉

• 18.4 hours 

Rotational Period

ESO/L. Calçada

Please talk to me about:

(Things I want to learn more about)

• Compact Binaries/Binary Evolution:

  • White Dwarfs Binaries and LISA
  • Common Envelope
  • Stripped Stars (e.g. sdB, WR, ...)
  • Products  of Binary Evolution (e.g. Barium Stars, R CrB, ELMs ...)
  • Halo vs Thick Disk Population (Gaia):
• Star Clusters (GCs     ):
  • LISA background
  • WD binaries in GCs (Binary Evolution)
• Time-Series Analysis:
  • Methods:
    • Gaussian Process
      • Flickering/QPOs/Magnetism in Symbiotics
    • Classification (unsupervised):
      • Dynamic time warping/The information bottleneck method
      • Where are all the AM CVns?

Evolutiocn Estrlar

Evolutiocn Estrlar

https://youtu.be/CouFXgUNK-M

https://pages.uoregon.edu/jimbrau/astr122-2015/Notes/Chapter20.html#lowm

Low Mass Star

Ciclo de Vida del Sol

Tipo G

https://www.astronomy.ohio-state.edu/thompson.1847/1144/Lecture15.html

Low Mass Star

Ciclo de Vida del Sol

Mirror Principle

Low Mass Star

Ciclo de Vida del Sol

Red Giant Branch

Low Mass Star

Ciclo de Vida del Sol

AGB

Low Mass Star

Ciclo de Vida del Sol

Planetary Nebula

Low Mass Star

Ciclo de Vida del Sol

White Dwarf

Low Mass Star

Ciclo de Vida del Sol

White Dwarf

Low Mass Star

Ciclo de Vida del Sol

White Dwarf

Low Mass Star

Clusters

https://youtu.be/wbvgjzW3Xz0

Manuel Pichardo Marcano (he/him)

Things I Love

Things I Hate

• Dominican Republic
• Astronomy
• Chess, Xiangqi, Shogi, Go
• Time-series/Light-Curves
• Globular Clusters
• Binary Evolution
• White Dwarfs

• Super Conservative Country
• No Dominican Astronomers
• Cooking (but love eating)
• TESS data systematics
• Crowded photometry (Dolphot)
• I love all Astro
• I love all Compact Objects

Caltech

AM CVn

Cataclysmic Variables

Accreting White Dwarf Binaries

Cataclysmic Variables

AM CVn

• Main Sequence Star
• P_orb ~ 80 min - 10 hours
• Outbursts:
  • 2-20 days
  • Disk instability model+ (DIM)
• >1000 in the galactic field
• Predicted large # in old Star Clusters

• White Dwarf/Helium Star
• P_orb ~ 5 - 70 min
• Outburts:
  • weeks?
  • DIM?
• ~70 in the galactic field

Mark A. Garlick

Caltech

AM Canum Venaticorum AM CVn

• White dwarf + White dwarf

• White dwarf + He Star

• Orbital Period: 5-70 minutes

• Rare: 70 Galactic field

Transiting Exoplanet Survey Satellite TESS

TESS Cadence and Coverage

• Primary mission:
  • 2-min selected targets
  • 30-min full-frame images (FFI).
• Extended:
  • 20 sec selected targets
  • 10-min FFI
• Second extended mission
  • 200-second FFI

Disk AM CVns

High state (high Ṁ)

• Hot ionized disk

~20

~10

~40-60 (?)

Low state (low Ṁ)

• Cold stable disk

Caltech

Outbursts

Pichardo Marcano et al. (2021)

SO duration

• Precursor
  • TESS (Duffy et al. 2021)
• 5/6 have Precursor
  • Except ASASSN-14cc

PTF1 J0719+4858

Pichardo Marcano et al. (2021)

ZTF

TESS

Precursor

Type of Super Outbursts

Osaki et al. (2005)

High Mass Ratio

DIM

Cataclysmic Variables

See also Duffy et al. (2021)

High Mass Ratio

High Mass Ratio

High Mass Ratio

 eccentric disc develops rapidly

Type of Echo Outbursts

SDSS J1043+5632

• P_orb = 28.5 min
• WZ Sge like
  • Precursors
  • EMT (Hameury+'20)
  • Reflection:
    • Hot Massive WD

• P_orb = 26.7 min
• Compare to TCP J21040470+4631129
  • EMT (Hameury+'20)
• Helium "SU UMa"
  • EMT+TTI (Kotko+'12)

SO

rebrightening

SO

rebrightening

• Color Evolution

PTF1 J0719+4858

Pichardo Marcano et al. (2021)

ZTF

SO

NO

SO

NO

rebrightening

rebrightening

Color Evolution

PTF1 J0719+4858

• Similar to Dwarf Novae

  • Hameury et al. (2020)

• Similar SDSS J1411+4812
  • Rivera Sandoval et al. (2021)
• Compare to SDSS 1137
  • Rivera Sandoval et al. (2021)

Pichardo Marcano et al. (2021)

SDSS J113732+405458

 Enhanced mass transfer

Rivera Sandoval et al. (2021)

P_orb = 26.7 min

P_orb ~ 60 min

Superoutburst duration vs P_orb

Pichardo Marcano et al. (2021)

Cataclysmic Variables

• White dwarf primary

• "Main-sequence" donor

• Roche-lobe overflow

• Accretion disk (non-magnetic)

• Highly Variables:

  • Dwarf novae

    • 2-8 mag outburst

    • 10-100 increase in L

Looking of CVs in GCs

NASA, ESA, H. Richer and J. Heyl (University of British Columbia), and J. Anderson and J. Kalirai (STScI)

Finding CVs in X-rays and UV

• Advantages of X-ray Searches:

  • Avoid crowding

• Disadvantages:

  • Small FoV (FUV)
  • Lx ≥ 10²⁹ ergs/s

Summary CVs in GCs

• Few of CVs per cluster

• X-ray biased sample:

  • Lx > 10²⁹ergs/s

• Dearth of DNe:

  • Only 17 confirmed

• Core-collapsed:

  • Bimodal population

• Non core-collapsed:

  • 1 faint population

• Period distribution?

  • 16 known periods

All Magnetics ?

• HST Archive
• 7 Globular Clusters
• Many Exposures
• Different properties
  • Metallicity
  • Core-collapsed
  • Non core-collapsed

SCOVaS: Survey for Compact Objects and Variables

Preliminary Results

NGC 6397

• Closest Core Collapse
• Second Closest
  • 2.4 kpc
  • 15 CV candidates
  • 2 Pulsars

Preliminary Results

NGC 6397

We haven't found new

X-ray faint CVs

Spoiler Alert!

Other Binaries

Credits: NASA/Rivera Sandoval

Main et al 2018 (Nature)

Redback 'spider' Pulsar

Redback  Pulsar

A new candidate Redback MSP

Pichardo Marcano et. al (2021a)

• Porb 1.96 days
• Longest Porb for Redback in GCs
• Missed MSP in Pulsar Searchers
  • Confirmed by Zhang et al. (2022)

Magnetic He WD Candidate

• V_rad > 150 km/s (MUSE)
• Not Detected in X-rays
  • Lx < 10²⁸ ergs/s
• Roche-lobe filling stripped star?
  • M~ 2 x 10^-4 ☉

• 18.4 hours 

Rotational Period

ESO/L. Calçada

Please talk to me about:

(Things I want to learn more about)

• Compact Binaries/Binary Evolution:

  • White Dwarfs Binaries and LISA
  • Common Envelope
  • Stripped Stars (e.g. sdB, WR, ...)
  • Products  of Binary Evolution (e.g. Barium Stars, R CrB, ELMs ...)
  • Halo vs Thick Disk Population (Gaia):
• Star Clusters (GCs     ):
  • LISA background
  • WD binaries in GCs (Binary Evolution)
• Time-Series Analysis:
  • Methods:
    • Gaussian Process
      • Flickering/QPOs/Magnetism in Symbiotics
    • Classification (unsupervised):
      • Dynamic time warping/The information bottleneck method
      • Where are all the AM CVns?

Also interested in:

• TESS:
  • Transients
  • Crowding
  • Symbiotics
• Halo vs Thick Disk:
  • Halo CVs
  • Halo AM CVns?

Data from Peters (2008)

Blue Variables

NGC 6397

• Pipeline to find interesting objects:
  • CMD Position and Periodicity/Variability Searches
• We were able to recover all known CV Candidates
• Found Orbital Period Redback Pulsar
• Detached White Dwarf-Red Dwarf
• First Magnetic He Core WD in GCs
• Many more variables to analyze...

Where are all the CVs?

Preliminary Results

M 92

• WFPC-2
• 2008-01-25 to 2008-01-30:
  • 76 Exposures
  • F555W
  • Exp time: 10 s

Preliminary Results

NGC 6397

• WFPC-2
• March-April 2005:
  • 126 orbits
  • F814W, F606W and F336W
  • Exp time: 500-700 s

He WD Candidate

 Pichardo Marcano et al. (2023)

HACKS CMD

 Data: Libralato et al. (2022)

Also interested in:

• Magnetic White Dwarfs:
  • A Magnetic Extremely Low-Mass WD in a Globular Cluster?
  • Magnetic WDs in Symbiotics from TESS:
    • Spin-up?

Data from Peters (2008)

• 18.4 hours 

• Halo vs Thick Disk:
  • Halo CVs:
    • Not Period Bouncers
  • Halo AM CVns

Pichardo Marcano et al. (2023)

Z And

28 min to 26.7 min in 20 Yr

He WD Candidate

Tracks from Althaus et al. (2009)

0.16 M☉

 0.22  M⊙

0.52 M⊙

• 18.4 hours 

He WD Candidate

Magnetic He WD Candidate

• Binary: Vrad > 150 km/s (MUSE)
• Not Detected in X-rays
  • Lx < 10²⁸ ergs/s
• Not an Roche-lobe filling stripped star
  • M~ 2 x 10^-4 ☉

• 18.4 hours 

Rotational Period

ESO/L. Calçada

He WD Candidate

 Pichardo Marcano et al. (2023)

MUSE spectrum

Data from Husser et al. (2016), Kamman et al. (2016)

• 5.3 hours 

Variable and No Hα Excess

• Not Detected in X-rays
• 0.2 Δmag in F336W
  
• No Hα in Excess
  
• Periodicity

  • 5.3 hours 

Variable WD Candidate

 Pichardo Marcano et al. (in prep.)

HUGS CMD

Data: Piotto et al.(2015)/ Nardiello et al. (2018)

Variable WD Candidate

 Pichardo Marcano et al. (in prep.)

HUGS CMD

Data: Piotto et al.(2015)/ Nardiello et al. (2018)

AM CVn Donors

van Roestel et al. 2022

q = M2/M1

0.0125 < q < 0.18

M2 = Donor

AM CVn Donors

Coleman et al. 2018

0.0125 < q < 0.18

<R_d> ~10¹⁰cm

q = M2/M1

AM CVn Donors

Coleman et al. 2018

0.0125 < q < 0.18

<R_d> ~10¹⁰cm

q = M2/M1

Mass-transfer rates vs orbital period

Mass-transfer rates vs orbital period

Magnetic He WD Candidate

 Pichardo Marcano et al. (2023)

• 18.4 hours

• 0.16 M☉

• 0.24 R☉
• 0.11 Gyr
• Teff 7586 K
• log g = 4.9

Other work with Accreting WDs

• Follow-up eROSITA transient:

• TESS time series analysis

• • Atel: Pichardo Marcano (2020)

  • Paper: Schwope, [...], Pichardo Marcano, et al. (2021)

Caltech

Compact Binaries Surveys

2- SCOVaS: Survey for Compact Objects and Variables

Pichardo Marcano et al. (2021a)

Pichardo Marcano et al. (2023)

   Pichardo Marcano et al. (in prep.)

1- TACOS: TESS AM CVn Outbursts Survey

Pichardo Marcano et al. (2021b)

Caltech

NASA

• Color Evolution

PTF1 J0719+4858

Pichardo Marcano et al. (2021)

ZTF

SO

NO

SO

NO

rebrightening

rebrightening

• Precursor
• Echo Outbursts
• DIM with Enhanced Mass Transfer  (e.g. Hameury & Lasota 2021)

SDSS J1043+5632

ZTF

TESS

• Precursor
• Echo Outbursts
• DIM with Enhanced Mass Transfer  (e.g. Hameury & Lasota 2021)

SDSS J1043+5632

ZTF

TESS

PTF1 J0719+4858:

• Similar to Dwarf Novae:
  • Hameury et al. (2020)
  • Rivera Sandoval et al. (2021)

Color Evolution

Pichardo Marcano et al. (2021)

Accreting White Dwarf Binaries

Cataclysmic Variables

AM CVn

• Main Sequence Star
• P_orb ~ 80 min - 10 hours
• Outbursts:
  • 2-20 days
  • Disk instability model+ (DIM)
• >1000 in the galactic field
• Predicted large # in old Star Clusters

• White Dwarf/Helium Star
• P_orb ~ 5 - 70 min
• Outburts:
  • weeks?
  • DIM?
• ~70 in the galactic field

Mark A. Garlick

Caltech

Color Evolution

PTF1 J0719+4858

• Similar to Dwarf Novae

  • Hameury et al. (2020)

• Similar SDSS J1411+4812
  • Rivera Sandoval et al. (2021)
• Compare to SDSS 1137
  • Rivera Sandoval et al. (2021)

Pichardo Marcano et al. (2021)

SDSS J113732+405458

 Enhanced mass transfer

Rivera Sandoval et al. (2021)

Color Evolution

PTF1 J0719+4858

SDSS J113732+405458

 Enhanced mass transfer

• Similar to Dwarf Novae

  • Hameury et al. (2020)

• Similar SDSS J1411+4812
  • Rivera Sandoval et al. (2021)
• Compare to SDSS 1137/SDSS 0807
  • Rivera Sandoval et al. (2021)

Pichardo Marcano et al. (2021)

Rivera Sandoval et al. (2021)

AM CVns

•  Helium Rich and Know to go into outburts

Normal Outbursts

V803 Cen

• WZ Sge like ?
  • Precursors
  • EMT (Hameury+'20)
  • Massive WD?

• Compare to TCP J21040470+4631129
  • EMT (Hameury+'20)
• Helium "SU UMa"
  • EMT+TTI (Kotko+'12)

AM Canum Venaticorum AM CVn

• White dwarf + White dwarf

• White dwarf + He Star

• Orbital Period: 5-70 minutes

• Rare: 70 Galactic field

Caltech

• P_orb 20 to ~ 60 minutes (?)

• Superoutburts (SO) and "Normal" outbursts (NO)

• Disk instability model (DIM)

  •  Constant Mass transfer rate

  • Tidal-thermal disk instability model

    • SO: Superhumps (periodic brightness variation )

Outbursting Systems

AM CVns

•  Helium Rich and (some) known to go into outbursts

Color Evolution

PTF1 J0719+4858

SS Cyg

Cataclysmic Variable

• Similar to Dwarf Novae

  • Hameury et al. (2020)

• Similar SDSS J1411+4812
  • Rivera Sandoval et al. (2021)
• Compare to SDSS 1137/SDSS 0807
  • Rivera Sandoval et al. (2021)

Pichardo Marcano et al. (2021)

Type of Super Outbursts

Osaki et al. (2005)

High Mass Ratio

DIM

Cataclysmic Variables

• Evolution Superhump

Pichardo Marcano et al. (2021)

Caltech

• Porb 20 to ~ 60 minutes (?)

• Superoutburts (SO) and "Normal" outbursts (NO)

  • SO: Superhumps (periodic brightness variation )

• Disk instability model (DIM)

  •  Constant Mass transfer rate

  • Tidal-thermal disk instability model

Outbursting Systems

Caltech

• Porb 20 to ~ 60 minutes (?)

• Superoutburts (SO) and "Normal" outbursts (NO)

• Disk instability model (DIM)

  •  Constant Mass transfer rate

  • Tidal-thermal disk instability model

    • SO: Superhumps (periodic brightness variation )

Outbursting Systems

Place Constraints

Constraint Empirical Relationships

1. T_rec ∝ P_orb^7.35
2. T_dur ∝ P_orb^4.54
3. Δ mag ∝ P_orb
4. Ground-Based:
   1. PTF/CRTS
   2. ZTF
   3. LINEAR

Levitan et al. 2015

See also Duffy et al. 2021

1. T_rec ∝ P_orb^7.35
2. T_dur ∝ P_orb^4.54
3. Δ mag ∝ P_orb
4. Ground-Based:
   1. PTF/CRTS
   2. ZTF
   3. LINEAR

Levitan et al. 2015

See also Duffy et al. 2021

Need detailed short-term variability

Constraint Empirical Relationships

Long-term monitoring

Pichardo Marcano et al. (2021)

• Orbital Periods:
  • 2-minute cadence
• Limits on Recurrence Time
• "Normal Outburts"

Type of Super Outbursts

Osaki et al. (2005)

High Mass Ratio

DIM

Cataclysmic Variables

Pichardo Marcano et al. (2021)

See also Duffy et al. (2021)